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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, De Rosa, G, Horne, Keith, Kriss, GA, Arav, N, Bentz, MC, Cackett, EM, Bontà, E Dalla, 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, De Lorenzo-Cáceres, A, 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, 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, Knigge, C, Krongold, Y, Lau, MW, Lee, JC, Leonard, DC, Li, Miao, Lira, P, Lochhaas, C, and Ma, Zhiyuan

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. Carnegie Supernova Project II: The Slowest Rising Type Ia Supernova LSQ14fmg and Clues to the Origin of Super-Chandrasekhar/03fg-like Events* * This paper includes data gathered with the 1 m Swope and 2.5 m du Pont telescopes at Las Campanas Observatory, Chile, and the Nordic Optical Telescope at the Observatorio del Roque de los Muchachos, La Palma, Spain.

Author

Hsiao, EY, Hoeflich, P, Ashall, C, Lu, J, Contreras, C, Burns, CR, Phillips, MM, Galbany, L, Anderson, JP, Baltay, C, Baron, E, Castellón, S, Davis, S, Freedman, Wendy L, Gall, C, Gonzalez, C, Graham, ML, Hamuy, M, Holoien, TW-S, Karamehmetoglu, E, Krisciunas, K, Kumar, S, Kuncarayakti, H, Morrell, N, Moriya, TJ, Nugent, PE, Perlmutter, S, Persson, SE, Piro, AL, Rabinowitz, D, Roth, M, Shahbandeh, M, Shappee, BJ, Stritzinger, MD, Suntzeff, NB, Taddia, F, and Uddin, SA

Subjects
Space Sciences, Physical Sciences, astro-ph.HE, astro-ph.GA, astro-ph.SR, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

The Type Ia supernova (SN Ia) LSQ14fmg exhibits exaggerated properties that may help to reveal the origin of the "super-Chandrasekhar"(or 03fg-like) group. The optical spectrum is typical of a 03fg-like SN Ia, but the light curves are unlike those of any SNe Ia observed. The light curves of LSQ14fmg rise extremely slowly. At -23 rest-frame days relative to B-band maximum, LSQ14fmg is already brighter than MV = -19 mag before host extinction correction. The observed color curves show a flat evolution from the earliest observation to approximately 1 week after maximum. The near-infrared light curves peak brighter than -20.5 mag in the J and H bands, far more luminous than any 03fg-like SNe Ia with near-infrared observations. At 1 month past maximum, the optical light curves decline rapidly. The early, slow rise and flat color evolution are interpreted to result from an additional excess flux from a power source other than the radioactive decay of the synthesized 56Ni. The excess flux matches the interaction with a typical superwind of an asymptotic giant branch (AGB) star in density structure, mass-loss rate, and duration. The rapid decline starting at around 1 month past B-band maximum may be an indication of rapid cooling by active carbon monoxide (CO) formation, which requires a low-temperature and high-density environment. These peculiarities point to an AGB progenitor near the end of its evolution and the core degenerate scenario as the likely explosion mechanism for LSQ14fmg.

Published
2020

4. 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

5. PS18kh: A New Tidal Disruption Event with a Non-axisymmetric Accretion Disk

Author

Holoien, TW-S, Huber, ME, Shappee, BJ, Eracleous, M, Auchettl, K, Brown, JS, Tucker, MA, Chambers, KC, Kochanek, CS, Stanek, KZ, Rest, A, Bersier, D, Post, RS, Aldering, G, Ponder, KA, Simon, JD, Kankare, E, Dong, D, Hallinan, G, Reddy, NA, Sanders, RL, Topping, MW, Bulger, J, Lowe, TB, Magnier, EA, Schultz, ASB, Waters, CZ, Willman, M, Wright, D, Young, DR, Dong, Subo, Prieto, JL, Thompson, Todd A, Denneau, L, Flewelling, H, Heinze, AN, Smartt, SJ, Smith, KW, Stalder, B, Tonry, JL, and Weiland, H

Subjects
Space Sciences, Physical Sciences, Astronomical Sciences, accretion accretion disks, black hole physics, galaxies: nuclei, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present the discovery of PS18kh, a tidal disruption event discovered at the center of SDSS J075654.53+341543.6 (d ≃ 322 Mpc) by the Pan-STARRS Survey for Transients. Our data set includes pre-discovery survey data from Pan-STARRS, the All-sky Automated Survey for Supernovae, and the Asteroid Terrestrial-impact Last Alert System as well as high-cadence, multiwavelength follow-up data from ground-based telescopes and Swift, spanning from 56 days before peak light until 75 days after. The optical/UV emission from PS18kh is well-fit as a blackbody with temperatures ranging from T ≃ 12,000 K to T ≃ 25,000 K and it peaked at a luminosity of L ≃ 8.8 × 1043 erg s-1. PS18kh radiated E = (3.45 ± 0.22) × 1050 erg over the period of observation, with (1.42 ± 0.20) × 1050 erg being released during the rise to peak. Spectra of PS18kh show a changing, boxy/double-peaked Hα emission feature, which becomes more prominent over time. We use models of non-axisymmetric accretion disks to describe the profile of the Hα line and its evolution. We find that at early times the high accretion rate leads the disk to emit a wind which modifies the shape of the line profile and makes it bell-shaped. At late times, the wind becomes optically thin, allowing the non-axisymmetric perturbations to show up in the line profile. The line-emitting portion of the disk extends from r in ∼ 60r g to an outer radius of r out ∼ 1400r g and the perturbations can be represented either as an eccentricity in the outer rings of the disk or as a spiral arm in the inner disk.

Published
2019

6. Investigation of Two Fermi-LAT Gamma-Ray Blazars Coincident with High-energy Neutrinos Detected by IceCube

Author

Garrappa, S, Buson, S, Franckowiak, A, Shappee, BJ, Beacom, JF, Dong, S, Holoien, TW-S, Kochanek, CS, Prieto, JL, Stanek, KZ, Thompson, TA, Aartsen, MG, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Auffenberg, J, Axani, S, Backes, P, Bagherpour, H, Bai, X, Barbano, A, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bohm, C, Börner, M, Böser, S, Botner, O, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bretz, H-P, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Carver, T, Chen, C, Cheung, E, Chirkin, D, Clark, K, Classen, L, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, de André, JPAM, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Dvorak, E, Eberhardt, B, Ehrhardt, T, Eller, P, Evenson, PA, Fahey, S, Fazely, AR, Felde, J, Filimonov, K, Finley, C, Friedman, E, Fritz, A, Gaisser, TK, Gallagher, J, and Ganster, E

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

After the identification of the gamma-ray blazar TXS 0506+056 as the first compelling IceCube neutrino source candidate, we perform a systematic analysis of all high-energy neutrino events satisfying the IceCube realtime trigger criteria. We find one additional known gamma-ray source, the blazar GB6 J1040+0617, in spatial coincidence with a neutrino in this sample. The chance probability of this coincidence is 30% after trial correction. For the first time, we present a systematic study of the gamma-ray flux, spectral and optical variability, and multiwavelength behavior of GB6 J1040+0617 and compare it to TXS 0506+056. We find that TXS 0506+056 shows strong flux variability in the Fermi-Large Area Telescope gamma-ray band, being in an active state around the arrival of IceCube-170922A, but in a low state during the archival IceCube neutrino flare in 2014/15. In both cases the spectral shape is statistically compatible (≤2σ) with the average spectrum showing no indication of a significant relative increase of a high-energy component. While the association of GB6 J1040+0617 with the neutrino is consistent with background expectations, the source appears to be a plausible neutrino source candidate based on its energetics and multiwavelength features, namely a bright optical flare and modestly increased gamma-ray activity. Finding one or two neutrinos originating from gamma-ray blazars in the given sample of high-energy neutrinos is consistent with previously derived limits of neutrino emission from gamma-ray blazars, indicating the sources of the majority of cosmic high-energy neutrinos remain unknown.

Published
2019

7. Velocity-resolved Reverberation Mapping of Five Bright Seyfert 1 Galaxies

Author

De Rosa, G, Fausnaugh, MM, Grier, CJ, Peterson, BM, Denney, KD, Horne, Keith, Bentz, MC, Ciroi, S, Bontà, E Dalla, Joner, MD, Kaspi, S, Kochanek, CS, Pogge, RW, Sergeev, SG, Vestergaard, M, Adams, SM, Antognini, J, Salvo, C Araya, Armstrong, E, Bae, J, Barth, AJ, Beatty, TG, Bhattacharjee, A, Borman, GA, Boroson, TA, Bottorff, MC, Brown, JE, Brown, JS, Brotherton, MS, Coker, CT, Clanton, C, Cracco, V, Crawford, SM, Croxall, KV, Eftekharzadeh, S, Eracleous, M, Fiorenza, SL, Frassati, A, Hawkins, K, Henderson, CB, Holoien, TW-S, Hutchison, T, Kellar, J, Kilerci-Eser, E, Kim, S, King, AL, La Mura, G, Laney, CD, Li, M, Lochhaas, C, Ma, Z, MacInnis, F, Manne-Nicholas, ER, Mason, M, McGraw, SM, Mogren, K, Montouri, C, Moody, JW, Mosquera, AM, Mudd, D, Musso, R, Nazarov, SV, Nguyen, ML, Ochner, P, Okhmat, DN, Onken, CA, Ou-Yang, B, Pancoast, A, Pei, L, Penny, M, Poleski, R, Portaluri, E, Prieto, J-L, Price-Whelan, AM, Pulatova, NG, Rafter, S, Roettenbacher, RM, Romero-Colmenero, E, Runnoe, J, Schimoia, JS, Shappee, BJ, Sherf, N, Simonian, GV, Siviero, A, Skowron, DM, Skowron, J, Somers, G, Spencer, M, Starkey, DA, Stevens, DJ, Stoll, R, Tamajo, E, Tayar, J, van Saders, JL, Valenti, S, Villanueva, S, Villforth, C, Weiss, Y, Winkler, H, and Zastrow, J

Subjects
galaxies: active, 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 the first results from a reverberation-mapping campaign undertaken during the first half of 2012, with additional data on one active galactic nucleus (AGN) (NGC 3227) from a 2014 campaign. Our main goals are (1) to determine the black hole masses from continuum-Hβ reverberation signatures, and (2) to look for velocity-dependent time delays that might be indicators of the gross kinematics of the broad-line region. We successfully measure Hβ time delays and black hole masses for five AGNs, four of which have previous reverberation mass measurements. The values measured here are in agreement with earlier estimates, though there is some intrinsic scatter beyond the formal measurement errors. We observe velocity-dependent Hβ lags in each case, and find that the patterns have changed in the intervening five years for three AGNs that were also observed in 2007.

Published
2018

8. Continuum Reverberation Mapping of the Accretion Disks in Two Seyfert 1 Galaxies

Author

Fausnaugh, MM, Starkey, DA, Horne, Keith, Kochanek, CS, Peterson, BM, Bentz, MC, Denney, KD, Grier, CJ, Grupe, D, Pogge, RW, De Rosa, G, Adams, SM, Barth, AJ, Beatty, Thomas G, Bhattacharjee, A, Borman, GA, Boroson, TA, Bottorff, MC, Brown, Jacob E, Brown, Jonathan S, Brotherton, MS, Coker, CT, Crawford, SM, Croxall, KV, Eftekharzadeh, Sarah, Eracleous, Michael, Joner, MD, Henderson, CB, Holoien, TW-S, Hutchison, T, Kaspi, Shai, Kim, S, King, Anthea L, Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, MacInnis, F, Manne-Nicholas, ER, Mason, M, Montuori, Carmen, Mosquera, Ana, Mudd, Dale, Musso, R, Nazarov, SV, Nguyen, ML, Okhmat, DN, Onken, Christopher A, Ou-Yang, B, Pancoast, A, Pei, L, Penny, Matthew T, Poleski, Radosław, Rafter, Stephen, Romero-Colmenero, E, Runnoe, Jessie, Sand, David J, Schimoia, Jaderson S, Sergeev, SG, Shappee, BJ, Simonian, Gregory V, Somers, Garrett, Spencer, M, Stevens, Daniel J, Tayar, Jamie, Treu, T, Valenti, Stefano, Van Saders, J, Villanueva, S, Villforth, C, Weiss, Yaniv, Winkler, H, and Zhu, W

Subjects
accretion, accretion disks, galaxies: individual, 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 optical continuum lags for two Seyfert 1 galaxies, MCG+08-11-011 and NGC 2617, using monitoring data from a reverberation mapping campaign carried out in 2014. Our light curves span the ugriz filters over four months, with median cadences of 1.0 and 0.6 days for MCG+08-11-011 and NGC 2617, respectively, combined with roughly daily X-ray and near-UV data from Swift for NGC 2617. We find lags consistent with geometrically thin accretion-disk models that predict a lag-wavelength relation of τ ∝ λ 4/3. However, the observed lags are larger than predictions based on standard thin-disk theory by factors of 3.3 for MCG+08-11-011 and 2.3 for NGC 2617. These differences can be explained if the mass accretion rates are larger than inferred from the optical luminosity by a factor of 4.3 in MCG+08-11-011 and a factor of 1.3 in NGC 2617, although uncertainty in the SMBH masses determines the significance of this result. While the X-ray variability in NGC 2617 precedes the UV/optical variability, the long (2.6 day) lag is problematic for coronal reprocessing models.

Published
2018

9. 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

10. Reverberation Mapping of Optical Emission Lines in Five Active Galaxies

Author

Fausnaugh, MM, Grier, CJ, Bentz, MC, Denney, KD, De Rosa, G, Peterson, BM, Kochanek, CS, Pogge, RW, Adams, SM, Barth, AJ, Beatty, Thomas G, Bhattacharjee, A, Borman, GA, Boroson, TA, Bottorff, MC, Brown, Jacob E, Brown, Jonathan S, Brotherton, MS, Coker, CT, Crawford, SM, Croxall, KV, Eftekharzadeh, Sarah, Eracleous, Michael, Joner, MD, Henderson, CB, Holoien, TW-S, Horne, Keith, Hutchison, T, Kaspi, Shai, Kim, S, King, Anthea L, Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, MacInnis, F, Manne-Nicholas, ER, Mason, M, Montuori, Carmen, Mosquera, Ana, Mudd, Dale, Musso, R, Nazarov, SV, Nguyen, ML, Okhmat, DN, Onken, Christopher A, Ou-Yang, B, Pancoast, A, Pei, L, Penny, Matthew T, Poleski, Radosław, Rafter, Stephen, Romero-Colmenero, E, Runnoe, Jessie, Sand, David J, Schimoia, Jaderson S, Sergeev, SG, Shappee, BJ, Simonian, Gregory V, Somers, Garrett, Spencer, M, Starkey, DA, Stevens, Daniel J, Tayar, Jamie, Treu, T, Valenti, Stefano, Van Saders, J, Villanueva, S, Villforth, C, Weiss, Yaniv, Winkler, H, and Zhu, W

Subjects
galaxies: active, galaxies: individual, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present the first results from an optical reverberation mapping campaign executed in 2014 targeting the active galactic nuclei (AGNs) MCG+08-11-011, NGC 2617, NGC 4051, 3C 382, and Mrk 374. Our targets have diverse and interesting observational properties, including a "changing look" AGN and a broad-line radio galaxy. Based on continuum-Hβ lags, we measure black hole masses for all five targets. We also obtain Hγ and He ii λ4686 lags for all objects except 3C 382. The He ii λ4686 lags indicate radial stratification of the BLR, and the masses derived from different emission lines are in general agreement. The relative responsivities of these lines are also in qualitative agreement with photoionization models. These spectra have extremely high signal-to-noise ratios (100-300 per pixel) and there are excellent prospects for obtaining velocity-resolved reverberation signatures.

Published
2017

11. Space Telescope and Optical Reverberation Mapping Project. V. Optical Spectroscopic Campaign and Emission-line Analysis for NGC 5548

Author

Pei, L, Fausnaugh, MM, Barth, AJ, Peterson, BM, Bentz, MC, De Rosa, G, Denney, KD, Goad, MR, Kochanek, CS, Korista, KT, Kriss, GA, Pogge, RW, Bennert, VN, Brotherton, M, Clubb, KI, Bontà, E Dalla, Filippenko, AV, Greene, JE, Grier, CJ, Vestergaard, M, Zheng, W, Adams, Scott M, Beatty, Thomas G, Bigley, A, Brown, Jacob E, Brown, Jonathan S, Canalizo, G, Comerford, JM, Coker, Carl T, Corsini, EM, Croft, S, Croxall, KV, Deason, AJ, Eracleous, Michael, Fox, OD, Gates, EL, Henderson, CB, Holmbeck, E, Holoien, TW-S, Jensen, JJ, Johnson, CA, Kelly, PL, Kim, S, King, A, Lau, MW, Li, Miao, Lochhaas, Cassandra, Ma, Zhiyuan, Manne-Nicholas, ER, Mauerhan, JC, Malkan, MA, McGurk, R, Morelli, L, Mosquera, Ana, Mudd, Dale, Sanchez, F Muller, Nguyen, ML, Ochner, P, Ou-Yang, B, Pancoast, A, Penny, Matthew T, Pizzella, A, Poleski, Radosław, Runnoe, Jessie, Scott, B, Schimoia, Jaderson S, Shappee, BJ, Shivvers, I, Simonian, Gregory V, Siviero, A, Somers, Garrett, Stevens, Daniel J, Strauss, MA, Tayar, Jamie, Tejos, N, Treu, T, Van Saders, J, Vican, L, Villanueva, S, Yuk, H, Zakamska, NL, Zhu, W, Anderson, MD, Arévalo, P, Bazhaw, C, Bisogni, S, Borman, GA, Bottorff, MC, Brandt, WN, Breeveld, AA, Cackett, EM, Carini, MT, Crenshaw, DM, De Lorenzo-Cáceres, A, Dietrich, M, Edelson, R, Efimova, NV, Ely, J, Evans, PA, and Ferland, GJ

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 the results of an optical spectroscopic monitoring program targeting NGC 5548 as part of a larger multiwavelength reverberation mapping campaign. The campaign spanned 6 months and achieved an almost daily cadence with observations from five ground-based telescopes. The Hβ and He ii λ4686 broad emission-line light curves lag that of the 5100 +-optical continuum by 4.17+0.36-0.36 and 0.79+0.35-0.34 days, respectively. The Hβ lag relative to the 1158 ultraviolet continuum light curve measured by the Hubble Space Telescope is ∼50% longer than that measured against the optical continuum, and the lag difference is consistent with the observed lag between the optical and ultraviolet continua. This suggests that the characteristic radius of the broad-line region is ∼50% larger than the value inferred from optical data alone. We also measured velocity-resolved emission-line lags for Hβ and found a complex velocity-lag structure with shorter lags in the line wings, indicative of a broad-line region dominated by Keplerian motion. The responses of both the Hβ and He ii emission lines to the driving continuum changed significantly halfway through the campaign, a phenomenon also observed for C iv, Lyα, He ii(+O iii]), and Si iv(+O iv]) during the same monitoring period. Finally, given the optical luminosity of NGC 5548 during our campaign, the measured Hβ lag is a factor of five shorter than the expected value implied by the R BLR-L AGN relation based on the past behavior of NGC 5548.

Published
2017

12. THE MAN BEHIND THE CURTAIN: X-RAYS DRIVE THE UV THROUGH NIR VARIABILITY IN THE 2013 ACTIVE GALACTIC NUCLEUS OUTBURST IN NGC 2617

Author

Shappee, BJ, Prieto, JL, Grupe, D, Kochanek, CS, Stanek, KZ, De Rosa, G, Mathur, S, Zu, Y, Peterson, BM, Pogge, RW, Komossa, S, Im, M, Jencson, J, Holoien, TW-S, Basu, U, Beacom, JF, Szczygieł, DM, Brimacombe, J, Adams, S, Campillay, A, Choi, C, Contreras, C, Dietrich, M, Dubberley, M, Elphick, M, Foale, S, Giustini, M, Gonzalez, C, Hawkins, E, Howell, DA, Hsiao, EY, Koss, M, Leighly, KM, Morrell, N, Mudd, D, Mullins, D, Nugent, JM, Parrent, J, Phillips, MM, Pojmanski, G, Rosing, W, Ross, R, Sand, D, Terndrup, DM, Valenti, S, Walker, Z, and Yoon, Y

Subjects
galaxies&COLFAML active, galaxies&COLFAML nuclei, galaxies&COLFAML Seyfert, line&COLFAML formation, line&COLFAML profiles, astro-ph.HE, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

After the All-Sky Automated Survey for SuperNovae discovered a significant brightening of the inner region of NGC 2617, we began a ∼70 day photometric and spectroscopic monitoring campaign from the X-ray through near-infrared (NIR) wavelengths. We report that NGC 2617 went through a dramatic outburst, during which its X-ray flux increased by over an order of magnitude followed by an increase of its optical/ultraviolet (UV) continuum flux by almost an order of magnitude. NGC 2617, classified as a Seyfert 1.8 galaxy in 2003, is now a Seyfert 1 due to the appearance of broad optical emission lines and a continuum blue bump. Such "changing look active galactic nuclei (AGNs)" are rare and provide us with important insights about AGN physics. Based on the Hβ line width and the radius-luminosity relation, we estimate the mass of central black hole (BH) to be (4 ± 1) × 107 M . When we cross-correlate the light curves, we find that the disk emission lags the X-rays, with the lag becoming longer as we move from the UV (2-3 days) to the NIR (6-9 days). Also, the NIR is more heavily temporally smoothed than the UV. This can largely be explained by a simple model of a thermally emitting thin disk around a BH of the estimated mass that is illuminated by the observed, variable X-ray fluxes. © 2014. The American Astronomical Society. All rights reserved..

Published
2014

13. Chandra, HST/STIS, NICER, Swift, and TESS Detail the Flare Evolution of the Repeating Nuclear Transient ASASSN-14ko

Author

Payne, AV, Auchettl, K, Shappee, BJ, Kochanek, CS, Boyd, PT, Holoien, TW-S, Fausnaugh, MM, Ashall, C, Hinkle, JT, Vallely, PJ, Stanek, KZ, Thompson, TA, Payne, AV, Auchettl, K, Shappee, BJ, Kochanek, CS, Boyd, PT, Holoien, TW-S, Fausnaugh, MM, Ashall, C, Hinkle, JT, Vallely, PJ, Stanek, KZ, and Thompson, TA

Abstract

ASASSN-14ko is a nuclear transient at the center of the AGN ESO 253−G003 that undergoes periodic flares. Optical flares were first observed in 2014 by the All-Sky Automated Survey for Supernovae (ASAS-SN) and their peak times are well-modeled with a period of 115.2 − 1.2 + 1.3 days and period derivative of −0.0026 ± 0.0006. Here we present ASAS-SN, Chandra, HST/STIS, NICER, Swift, and TESS data for the flares that occurred on 2020 December, 2021 April, 2021 July, and 2021 November. These four flares represent flares 18–21 of the total number of flares observed by ASAS-SN so far since 2014. The HST/STIS UV spectra evolve from blueshifted broad absorption features to redshifted broad emission features over ∼10 days. The Swift UV/optical light curves peaked as predicted by the timing model, but the peak UV luminosities that varied between flares and the UV flux in Flare 20 were roughly half the brightness of the other peaks. The X-ray luminosities consistently decreased and the spectra became harder during the UV/optical rise, but apparently without changes in absorption. Finally, two high-cadence TESS light curves from Flare 18 and Flare 12 showed that the slopes during the rising and declining phases changed over time, which indicates some stochasticity in the flare’s driving mechanism. Although ASASSN-14ko remains observationally consistent with a repeating partial tidal disruption event, these rich multi-wavelength data are in need of a detailed theoretical model.

Published
2023

14. The Rapid X-Ray and UV Evolution of ASASSN-14ko

Author

Payne, A, Shappee, BJ, Hinkle, JT, Holoien, TW-S, Auchettl, K, Kochanek, CS, Stanek, KZ, Thompson, TA, Tucker, MA, Armstrong, JD, Boyd, PT, Brimacombe, J, Cornect, R, Huber, ME, Jha, SW, Lin, C-C, Payne, A, Shappee, BJ, Hinkle, JT, Holoien, TW-S, Auchettl, K, Kochanek, CS, Stanek, KZ, Thompson, TA, Tucker, MA, Armstrong, JD, Boyd, PT, Brimacombe, J, Cornect, R, Huber, ME, Jha, SW, and Lin, C-C

Abstract

ASASSN-14ko is a recently discovered periodically flaring transient at the center of the active galactic nucleus (AGN) ESO 253−G003 with a slowly decreasing period. Here, we show that the flares originate from the northern, brighter nucleus in this dual-AGN, post-merger system. The light curves for the two flares that occurred in 2020 May and September are nearly identical over all wavelengths. For both events, Swift observations showed that the UV and optical wavelengths brightened in unison. The effective temperature of the UV/optical emission rises and falls with the increase and subsequent decline in the luminosity. The X-ray flux, by contrast, first rapidly drops over ∼2.6 days, rises for ∼5.8 days, drops again over ∼4.3 days, and then recovers. The X-ray spectral evolution of the two flares differ, however. During the 2020 May peak the spectrum softened with increases in the X-ray luminosity, while we observed the reverse for the 2020 September peak. We found a small change in the period derivative, which seems to indicate that the system does not have a static period derivative and there is some stochasticity in its evolution.

Published
2022

15. Investigating the Nature of the Luminous Ambiguous Nuclear Transient ASASSN-17jz

Author

Holoien, TW-S, Neustadt, JMM, Vallely, PJ, Auchettl, K, Hinkle, JT, Romero-Canizales, C, Shappee, BJ, Kochanek, CS, Stanek, KZ, Chen, P, Dong, S, Prieto, JL, Thompson, TA, Brink, TG, Filippenko, A, Zheng, W, Bersier, D, Bose, S, Burgasser, AJ, Channa, S, de Jaeger, T, Hestenes, J, Im, M, Jeffers, B, Jun, HD, Lansbury, G, Post, RS, Ross, TW, Stern, D, Tang, K, Tucker, MA, Valenti, S, Yunus, S, Zhang, KD, Holoien, TW-S, Neustadt, JMM, Vallely, PJ, Auchettl, K, Hinkle, JT, Romero-Canizales, C, Shappee, BJ, Kochanek, CS, Stanek, KZ, Chen, P, Dong, S, Prieto, JL, Thompson, TA, Brink, TG, Filippenko, A, Zheng, W, Bersier, D, Bose, S, Burgasser, AJ, Channa, S, de Jaeger, T, Hestenes, J, Im, M, Jeffers, B, Jun, HD, Lansbury, G, Post, RS, Ross, TW, Stern, D, Tang, K, Tucker, MA, Valenti, S, Yunus, S, and Zhang, KD

Abstract

We present observations of the extremely luminous but ambiguous nuclear transient (ANT) ASASSN-17jz, spanning roughly 1200 days of the object’s evolution. ASASSN-17jz was discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN) in the galaxy SDSS J171955.84+414049.4 on UT 2017 July 27 at a redshift of z = 0.1641. The transient peaked at an absolute B-band magnitude of M B,peak = −22.81, corresponding to a bolometric luminosity of L bol,peak = 8.3 × 1044 erg s−1, and exhibited late-time ultraviolet emission that was still ongoing in our latest observations. Integrating the full light curve gives a total emitted energy of E tot = (1.36 ±0.08) × 1052 erg, with (0.80 ± 0.02) × 1052 erg of this emitted within 200 days of peak light. This late-time ultraviolet emission is accompanied by increasing X-ray emission that becomes softer as it brightens. ASASSN-17jz exhibited a large number of spectral emission lines most commonly seen in active galactic nuclei (AGNs) with little evidence of evolution. It also showed transient Balmer features, which became fainter and broader over time, and are still being detected >1000 days after peak brightness. We consider various physical scenarios for the origin of the transient, including supernovae (SNe), tidal disruption events, AGN outbursts, and ANTs. We find that the most likely explanation is that ASASSN-17jz was a SN IIn occurring in or near the disk of an existing AGN, and that the late-time emission is caused by the AGN transitioning to a more active state.

Published
2022

16. SN2017jgh: a high-cadence complete shock cooling light curve of a SN IIb with the Kepler telescope

Author

Armstrong, P, Tucker, BE, Rest, A, Ridden-Harper, R, Zenati, Y, Piro, AL, Hinton, S, Lidman, C, Margheim, S, Narayan, G, Shaya, E, Garnavich, P, Kasen, D, Villar, V, Zenteno, A, Arcavi, I, Drout, M, Foley, RJ, Wheeler, J, Anais, J, Campillay, A, Coulter, D, Dimitriadis, G, Jones, D, Kilpatrick, CD, Munoz-Elgueta, N, Rojas-Bravo, C, Vargas-Gonzalez, J, Bulger, J, Chambers, K, Huber, M, Lowe, T, Magnier, E, Shappee, BJ, Smartt, S, Smith, KW, Barclay, T, Barentsen, G, Dotson, J, Gully-Santiago, M, Hedges, C, Howell, S, Cody, A, Auchettl, K, Bodi, A, Bognar, Z, Brimacombe, J, Brown, P, Cseh, B, Galbany, L, Hiramatsu, D, Holoien, TW-S, Howell, DA, Jha, SW, Konyves-Toth, R, Kriskovics, L, McCully, C, Milne, P, Munoz, J, Pan, Y, Pal, A, Sai, H, Sarneczky, K, Smith, N, Sodor, A, Szabo, R, Szakats, R, Valenti, S, Vinko, J, Wang, X, Zhang, K, Zsidi, G, Armstrong, P, Tucker, BE, Rest, A, Ridden-Harper, R, Zenati, Y, Piro, AL, Hinton, S, Lidman, C, Margheim, S, Narayan, G, Shaya, E, Garnavich, P, Kasen, D, Villar, V, Zenteno, A, Arcavi, I, Drout, M, Foley, RJ, Wheeler, J, Anais, J, Campillay, A, Coulter, D, Dimitriadis, G, Jones, D, Kilpatrick, CD, Munoz-Elgueta, N, Rojas-Bravo, C, Vargas-Gonzalez, J, Bulger, J, Chambers, K, Huber, M, Lowe, T, Magnier, E, Shappee, BJ, Smartt, S, Smith, KW, Barclay, T, Barentsen, G, Dotson, J, Gully-Santiago, M, Hedges, C, Howell, S, Cody, A, Auchettl, K, Bodi, A, Bognar, Z, Brimacombe, J, Brown, P, Cseh, B, Galbany, L, Hiramatsu, D, Holoien, TW-S, Howell, DA, Jha, SW, Konyves-Toth, R, Kriskovics, L, McCully, C, Milne, P, Munoz, J, Pan, Y, Pal, A, Sai, H, Sarneczky, K, Smith, N, Sodor, A, Szabo, R, Szakats, R, Valenti, S, Vinko, J, Wang, X, Zhang, K, and Zsidi, G

Abstract

SN 2017jgh is a type IIb supernova discovered by Pan-STARRS during the C16/C17 campaigns of the Kepler/K2 mission. Here, we present the Kepler/K2 and ground based observations of SN 2017jgh, which captured the shock cooling of the progenitor shock breakout with an unprecedented cadence. This event presents a unique opportunity to investigate the progenitors of stripped envelope supernovae. By fitting analytical models to the SN 2017jgh light curve, we find that the progenitor of SN 2017jgh was likely a yellow supergiant with an envelope radius of $\sim 50{\!-\!}290\, {\rm R}_{\odot }$, and an envelope mass of $\sim 0{\!-\!}1.7\, {\rm M}_{\odot }$. SN 2017jgh likely had a shock velocity of ∼7500−10 300 km s−1. Additionally, we use the light curve of SN 2017jgh to investigate how early observations of the rise contribute to constraints on progenitor models. Fitting just the ground based observations, we find an envelope radius of $\sim 50{\!-\!}330\, {\rm R}_{\odot }$, an envelope mass of $\sim 0.3{\!-\!}1.7\, {\rm M}_{\odot }$ and a shock velocity of ∼9000−15 000 km s−1. Without the rise, the explosion time cannot be well constrained that leads to a systematic offset in the velocity parameter and larger uncertainties in the mass and radius. Therefore, it is likely that progenitor property estimates through these models may have larger systematic uncertainties than previously calculated.

Published
2021

17. Seeing Double:ASASSN-18bt Exhibits a Two-Component Rise in the Early-Time K2 Light Curve

Author

Shappee, BJ, Holoien, TW-S, Drout, MR, Auchettl, K, Stritzinger, MD, Kochanek, CS, Stanek, KZ, Shaya, E, Narayan, G, Brown, JS, Bose, S, Bersier, D, Brimacombe, J, Chen, P, Dong, S, Holmbo, S, Katz, B, Munoz, JA, Mutel, RL, Post, RS, Prieto, JL, Shields, J, Tallon, D, Thompson, TA, Vallely, PJ, Villanueva, S, Denneau, L, Flewelling, H, Heinze, AN, Smith, KW, Stalder, B, Tonry, JL, Weiland, H, Barclay, T, Barentsen, G, Cody, AM, Dotson, J, Foerster, F, Garnavich, P, Gully-Santiago, M, Hedges, C, Howell, S, Kasen, D, Margheim, S, Mushotzky, R, Rest, A, Tucker, BE, Villar, A, Zenteno, A, Beerman, G, Bjella, R, Castillo, G, Coughlin, J, Elsaesser, B, Flynn, S, Gangopadhyay, R, Griest, K, Hanley, M, Kampmeier, J, Kloetzel, R, Kohnert, L, Labonde, C, Larsen, R, Larson, KA, McCalmont-Everton, KM, McGinn, C, Migliorini, L, Moffatt, J, Muszynski, M, Nystrom, V, Osborne, D, Packard, M, Peterson, CA, Redick, M, Reedy, LH, Ross, SE, Spencer, B, Steward, K, Van Cleve, JE, Vinicius de Miranda Cardoso, J, Weschler, T, Wheaton, A, Bulger, J, Chambers, KC, Flewelling, HA, Huber, ME, Lowe, TB, Magnier, EA, Schultz, ASB, Waters, CZ, Willman, M, Baron, E, Chen, Z, Derkacy, JM, Huang, F, Li, L, Li, W, Li, X, Mo, J, Rui, L, Sai, H, Wang, L, Wang, X, Xiang, D, Zhang, J, Zhang, K, Zhang, T, Zhang, X, Zhao, X, Brown, PJ, Hermes, JJ, Nordin, J, Points, S, Sodor, A, and Strampelli, GM

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Field (physics), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, individual (ASASSN-18bt, SN 2018oh) [supernovae], Light curve, 01 natural sciences, Power law, Redshift, Supernova, Apparent magnitude, 13. Climate action, Space and Planetary Science, Asteroid, 0103 physical sciences, QD, 010306 general physics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, QC, QB
Abstract

On 2018 Feb. 4.41, the All-Sky Automated Survey for SuperNovae (ASAS-SN) discovered ASASSN-18bt in the K2 Campaign 16 field. With a redshift of z=0.01098 and a peak apparent magnitude of B_{max}=14.31, ASASSN-18bt is the nearest and brightest SNe Ia yet observed by the Kepler spacecraft. Here we present the discovery of ASASSN-18bt, the K2 light curve, and pre-discovery data from ASAS-SN and the Asteroid Terrestrial-impact Last Alert System (ATLAS). The K2 early-time light curve has an unprecedented 30-minute cadence and photometric precision for an SN~Ia light curve, and it unambiguously shows a ~4 day nearly linear phase followed by a steeper rise. Thus, ASASSN-18bt joins a growing list of SNe Ia whose early light curves are not well described by a single power law. We show that a double-power-law model fits the data reasonably well, hinting that two physical processes must be responsible for the observed rise. However, we find that current models of the interaction with a non-degenerate companion predict an abrupt rise and cannot adequately explain the initial, slower linear phase. Instead, we find that existing, published models with shallow 56Ni are able to span the observed behavior and, with tuning, may be able to reproduce the ASASSN-18bt light curve. Regardless, more theoretical work is needed to satisfactorily model this and other early-time SNe~Ia light curves. Finally, we use Swift X-ray non-detections to constrain the presence of circumstellar material (CSM) at much larger distances and lower densities than possible with the optical light curve. For a constant density CSM these non-detections constrain rho, 17 pages, 8 figures, 3 Tables. Accepted to ApJ. This work is part of a number of papers analyzing ASASSN-18bt, with coordinated papers from Dimitriadis et al. (2018) and Li et al. (2018)

Published
2019
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18. ASASSN-15lh: A highly super-luminous supernova

Author

Dong, S, Shappee, BJ, Prieto, JL, Jha, SW, Stanek, KZ, Holoien, TW-S, Kochanek, CS, Thompson, TA, Morrell, N, Thompson, IB, Basu, U, Beacom, JF, Bersier, D, Brimacombe, J, Brown, JS, Chen, P, Conseil, E, Danilet, AB, Falco, E, Grupe, D, Kiyota, S, Masi, G, Nicholls, B, Olivares, F, Pignata, G, Pojmanski, G, Simonian, GV, Szczygiel, DM, and Wozniak, PR

Subjects
QB
Abstract

We report the discovery and early evolution of ASASSN-15lh, the most luminous supernova ever found. At redshift z=0.2326, ASASSN-15lh reached an absolute magnitude of M_{u,AB} ~ -23.5 and bolometric luminosity L_bol ~ 2.2x10^45 ergs/s, which is >~ 2 times more luminous than any previously known supernova. Its spectra match the hydrogen-poor sub-class of super-luminous supernovae (SLSNe-I), whose energy sources and progenitors are poorly understood. In contrast to known SLSNe-I, most of which reside in star-forming, dwarf galaxies, its host appears to be a luminous galaxy (M_V ~ -22; M_K ~ -25.1) with little star formation. In the two months since its first detection, ASASSN-15lh has radiated ~7.5x10^51 ergs, challenging the popular magnetar model for the engine of SLSNe-I.

19. ASASSN-18di: discovery of a $ΔV \sim 10$ flare on a mid-M dwarf

Author

Rodríguez, R, Schmidt, SJ, Jayasinghe, T, Stanek, KZ, Prieto, JL, Shappee, B, Kochanek, CS, Thompson, TA, Shields, J, Holoien, TW-S, Bersier, D, and Brimacombe, J

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB
Abstract

We report and characterize a white-light superflare on a previously undiscovered M dwarf detected by the ASAS-SN survey. Employing various color-magnitude and color-spectral type relationships, we estimate several stellar parameters, including the quiescent V-band magnitude, from which we derive a flare amplitude of $\Delta V \sim 10$. We determine an r-band absolute magnitude of $M_{r} = 11.4$, consistent with a mid-M dwarf, and an approximate distance to the source of $2.2$ kpc. Using classical-flare models, we infer a flare energy of $E_{V} \simeq (4.1\pm 2.2)\times 10^{36}$ ergs, making this one of the strongest flares documented on an M dwarf.

20. Supernova progenitors, their variability and the Type IIP Supernova ASASSN-16fq in M66

Author

Kochanek, CS, Fraser, M, Adams, SM, Sukhbold, T, Prieto, JL, Muller, T, Bock, G, Brown, JS, Dong, S, Holoien, TW-S, Khan, R, Shappee, BJ, and Stanek, KZ

Subjects
stars: massive, supernovae: general, 13. Climate action, 7. Clean energy, supernovae: individual: SN 2016cok, galaxies: individual: M 66
Abstract

We identify a pre-explosion counterpart to the nearby Type IIP supernova ASASSN-16fq (SN 2016cok) in archival $\textit{Hubble Space Telescope}$ data. The source appears to be a blend of several stars that prevents obtaining accurate photometry. However, with reasonable assumptions about the stellar temperature and extinction, the progenitor almost certainly had an initial mass $M_*$ $\lesssim$ 17 M$_\odot$, and was most likely in the mass range of $M_*$ = 8–12 M$_\odot$. Observations once ASASSN-16fq has faded will have no difficulty accurately determining the properties of the progenitor. In 8 yr of Large Binocular Telescope (LBT) data, no significant progenitor variability is detected to rms limits of roughly 0.03 mag. Of the six nearby supernova (SN) with constraints on the low-level variability, SN 1987A, SN 1993J, SN 2008cn, SN 2011dh, SN 2013ej and ASASSN-16fq, only the slowly fading progenitor of SN 2011dh showed clear evidence of variability. Excluding SN 1987A, the 90 per cent confidence limit implied by these sources on the number of outbursts over the last decade before the SN that last longer than 0.1 yr (full width at half-maximum) and are brighter than $M_R$ < −8 mag is approximately $N_\text{out}$ $\lesssim$ 3. Our continuing LBT monitoring programme will steadily improve constraints on pre-SN progenitor variability at amplitudes far lower than achievable by SN surveys., CSK, KZS, JSB, SMA and TWSH are supported by NSF grants AST-1515876 and AST-1515927. BJS is supported by NASA through Hubble Fellowship grant HF-51348.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. TW-SH is supported by the DOE Computational Science Graduate Fellowship, grant number DE-FG02- 97ER25308. TS is partly supported by NSF grant PHY-1404311 to J. Beacom. This work was partly supported by the European Union FP7 programme through ERC grant number 320360. Support for JLP is provided in part by FONDECYT through the grant 1151445 and by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. SD is supported by the Strategic Priority Research Program ‘The Emergence of Cosmological Structures’ of the Chinese Academy of Sciences (Grant No. XDB09000000) and NSFC project 11573003. Some of the observations were carried out using the LBT at Mt Graham, AZ. The LBT is an international collaboration among institutions in the United States, Italy and Germany. LBT Corporation partners are the University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max–Planck Society, the Astrophysical Institute Potsdam and Heidelberg University; the Ohio State University; and The Research Corporation, on behalf of the University of Notre Dame, University of Minnesota and University of Virginia. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, and in part on observations made with the NASA/ESA HST obtained at the Space Telescope Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Some observations were obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA).

21. Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo

Author

The LIGO Scientific Collaboration, The Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Ar��ne, M., Arnaud, N., Aronson, S. M., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baird, J., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Bals, A., Banagiri, S., Barayoga, J. C., Barbieri, C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., B��csy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Benjamin, M. G., Bergmann, G., Bernuzzi, S., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Biggs, E., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bobba, F., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calder��n, Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Canepa, M., Cannon, K. C., Cao, H., Cao, J., Carapella, G., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavagli��, M., Cavalier, F., Cavalieri, R., Cella, G., Cerd��-Dur��n, P., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chiadini, F., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Cie��lar, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Coccia, E., Cohadon, P. -F., Cohen, D., Colleoni, M., Collette, C. G., Collins, C., Colpi, M., Cominsky, L. R., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carri��n, I., Corezzi, S., Corley, K. R., Cornish, N., Corre, D., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, D��lya, G., D'Angelo, B., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Del��glise, S., Del Pozzo, W., DeMarchi, L. M., Demos, N., Dent, T., De Pietri, R., De Rosa, R., De Rossi, C., DeSalvo, R., de Varona, O., Dhurandhar, S., D��az, M. C., Dietrich, T., Di Fiore, L., DiFronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Durante, O., Dwyer, S. E., Easter, P. J., Eddolls, G., Edo, T. B., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Errico, L., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fishner, J. M., Fittipaldi, R., Fitz-Axen, M., Fiumara, V., Flaminio, R., Fletcher, M., Floden, E., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Vivanco, Francisco Hernandez, Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fronz��, G., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garc��a-Quir��s, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gill, K., Glover, L., Gniesmer, J., Godwin, P., Goetz, E., Goetz, R., Goncharov, B., Gonz��lez, G., Castro, J. M. Gonzalez, Gopakumar, A., Gossan, S. E., Gosselin, M., Gouaty, R., Grace, B., Grado, A., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Grimaldi, A., Grimm, S. J., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Gulati, H. K., Guo, Y., Gupta, A., Gupta, Anchal, Gupta, P., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hasskew, R. K., Haster, C. J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hellman, F., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heurs, M., Hild, S., Hinderer, T., Hochheim, S., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Huang, Y., H��bner, M. T., Huerta, E. A., Huet, D., Hughey, B., Hui, V., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Inchauspe, H., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. I., Jones, J. D., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., K��f��lian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. H., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kovalam, M., Kozak, D. B., Kr��mer, C., Kringel, V., Krishnendu, N., Kr��lak, A., Krupinski, N., Kuehn, G., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Laghi, D., Lai, K. H., Lam, T. L., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lenon, A. K., Leroy, N., Letendre, N., Levin, Y., Li, A., Li, J., Li, K. J. L., Li, T. G. 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S., Kouprianov, V., Prieto, J. L., Reichart, D. E., Salemi, F., Sand, D. J., Shappee, B. J., Stanek, K. Z., Tartaglia, L., Valenti, S., Wyatt, S., Yang, S., RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, RS: FSE MSP, Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du 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(LKB [Collège de France]), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Collège de France (CdF)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lumière Matière [Villeurbanne] (ILM), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, ESPCI ParisTech, Institut de Physique Nucléaire de Lyon (IPNL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), LIGO Scientific, Virgo, Abbott, Bp, Abbott, R, Abbott, Td, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adya, Vb, Affeldt, C, Agathos, M, Agatsuma, K, 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Subjects
Astronomy, PROGENITOR, Gravitational Wave, II-P SUPERNOVA, Astrophysics, Burst GW detection, 7. Clean energy, 01 natural sciences, General Relativity and Quantum Cosmology, gravitational waves, supernovae, Physics, Particles & Fields, neutrino, Gravitational waves, Novae and supernovae, gravitational radiation: energy, LIGO, QC, QB, Settore FIS/01, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), CURVE, ii-p supernova, energy: emission, neutrino burst, NEUTRINO BURST, bar-mode instability, Core-Collapse Supernovae, Novae and supernovae, Supernova, General relativity, Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], simulations, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Advanced Virgo, stars, Gravitational waves sources, data analysis, SHOCK BREAKOUT, gr-qc, supernova: collapse, Astrophysics::High Energy Astrophysical Phenomena, alternative theories of gravity, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, emission: model, Gravitational waves, Settore FIS/05 - Astronomia e Astrofisica, Coincident, 0103 physical sciences, Advanced LIGO, ddc:530, SDG 7 - Affordable and Clean Energy, 010306 general physics, numerical calculations, curve, STFC, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, Virgo, RCUK, progenitor, SIMULATIONS, radiation, BAR-MODE INSTABILITY, Stars, VIRGO, Physics and Astronomy, explosion mechanism, Orders of magnitude (time), shock breakout, 13. Climate action, efficiency, gravitational radiation: emission, RADIATION, EXPLOSION MECHANISM, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, higher-dimensional, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], STARS, Gravitational Waves
Abstract

We present the results from a search for gravitational-wave transients associated with core-collapse supernovae observed within a source distance of approximately 20 Mpc during the first and second observing runs of Advanced LIGO and Advanced Virgo. No significant gravitational-wave candidate was detected. We report the detection efficiencies as a function of the distance for waveforms derived from multidimensional numerical simulations and phenomenological extreme emission models. For neutrino-driven explosions the distance at which we reach 50% detection efficiency is approaching 5 kpc, and for magnetorotationally-driven explosions is up to 54 kpc. However, waveforms for extreme emission models are detectable up to 28 Mpc. For the first time, the gravitational-wave data enabled us to exclude part of the parameter spaces of two extreme emission models with confidence up to 83%, limited by coincident data coverage. Besides, using ad hoc harmonic signals windowed with Gaussian envelopes we constrained the gravitational-wave energy emitted during core-collapse at the levels of $4.27\times 10^{-4}\,M_\odot c^2$ and $1.28\times 10^{-1}\,M_\odot c^2$ for emissions at 235 Hz and 1304 Hz respectively. These constraints are two orders of magnitude more stringent than previously derived in the corresponding analysis using initial LIGO, initial Virgo and GEO 600 data., Comment: 13 pages, 5 figures

Published
2020
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22. A case for a binary black hole system revealed via quasi-periodic outflows.

Author

Pasham DR, Tombesi F, Suková P, Zajaček M, Rakshit S, Coughlin E, Kosec P, Karas V, Masterson M, Mummery A, Holoien TW, Guolo M, Hinkle J, Ripperda B, Witzany V, Shappee B, Kara E, Horesh A, van Velzen S, Sfaradi I, Kaplan D, Burger N, Murphy T, Remillard R, Steiner JF, Wevers T, Arcodia R, Buchner J, Merloni A, Malyali A, Fabian A, Fausnaugh M, Daylan T, Altamirano D, Payne A, and Ferraraa EC

Abstract

Binaries containing a compact object orbiting a supermassive black hole are thought to be precursors of gravitational wave events, but their identification has been extremely challenging. Here, we report quasi-periodic variability in x-ray absorption, which we interpret as quasi-periodic outflows (QPOuts) from a previously low-luminosity active galactic nucleus after an outburst, likely caused by a stellar tidal disruption. We rule out several models based on observed properties and instead show using general relativistic magnetohydrodynamic simulations that QPOuts, separated by roughly 8.3 days, can be explained with an intermediate-mass black hole secondary on a mildly eccentric orbit at a mean distance of about 100 gravitational radii from the primary. Our work suggests that QPOuts could be a new way to identify intermediate/extreme-mass ratio binary candidates.

Published
2024
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23. Response to Comment on "A noninteracting low-mass black hole-giant star binary system".

Author

Thompson TA, Kochanek CS, Stanek KZ, Badenes C, Jayasinghe T, Tayar J, Johnson JA, Holoien TW, Auchettl K, and Covey K

Abstract

Van den Heuvel and Tauris argue that if the red giant star in the system 2MASS J05215658+4359220 has a mass of 1 solar mass ( M ☉ ), then its unseen companion could be a binary composed of two 0.9 M ☉ stars, making a triple system. We contend that the existing data are most consistent with a giant of mass [Formula: see text] M ☉ , implying a black hole companion of [Formula: see text] M ☉ ., (Copyright © 2020, American Association for the Advancement of Science.)

Published
2020
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24. A noninteracting low-mass black hole-giant star binary system.

Author

Thompson TA, Kochanek CS, Stanek KZ, Badenes C, Post RS, Jayasinghe T, Latham DW, Bieryla A, Esquerdo GA, Berlind P, Calkins ML, Tayar J, Lindegren L, Johnson JA, Holoien TW, Auchettl K, and Covey K

Abstract

Black hole binary systems with companion stars are typically found via their x-ray emission, generated by interaction and accretion. Noninteracting binaries are expected to be plentiful in the Galaxy but must be observed using other methods. We combine radial velocity and photometric variability data to show that the bright, rapidly rotating giant star 2MASS J05215658+4359220 is in a binary system with a massive unseen companion. The system has an orbital period of ~83 days and near-zero eccentricity. The photometric variability period of the giant is consistent with the orbital period, indicating star spots and tidal synchronization. Constraints on the giant's mass and radius imply that the unseen companion is [Formula: see text] solar masses, indicating that it is a noninteracting low-mass black hole or an unexpectedly massive neutron star., (Copyright © 2019 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works.)

Published
2019
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25. Light curves of the neutron star merger GW170817/SSS17a: Implications for r-process nucleosynthesis.

Author

Drout MR, Piro AL, Shappee BJ, Kilpatrick CD, Simon JD, Contreras C, Coulter DA, Foley RJ, Siebert MR, Morrell N, Boutsia K, Di Mille F, Holoien TW, Kasen D, Kollmeier JA, Madore BF, Monson AJ, Murguia-Berthier A, Pan YC, Prochaska JX, Ramirez-Ruiz E, Rest A, Adams C, Alatalo K, Bañados E, Baughman J, Beers TC, Bernstein RA, Bitsakis T, Campillay A, Hansen TT, Higgs CR, Ji AP, Maravelias G, Marshall JL, Bidin CM, Prieto JL, Rasmussen KC, Rojas-Bravo C, Strom AL, Ulloa N, Vargas-González J, Wan Z, and Whitten DD

Abstract

On 17 August 2017, gravitational waves (GWs) were detected from a binary neutron star merger, GW170817, along with a coincident short gamma-ray burst, GRB 170817A. An optical transient source, Swope Supernova Survey 17a (SSS17a), was subsequently identified as the counterpart of this event. We present ultraviolet, optical, and infrared light curves of SSS17a extending from 10.9 hours to 18 days postmerger. We constrain the radioactively powered transient resulting from the ejection of neutron-rich material. The fast rise of the light curves, subsequent decay, and rapid color evolution are consistent with multiple ejecta components of differing lanthanide abundance. The late-time light curve indicates that SSS17a produced at least ~0.05 solar masses of heavy elements, demonstrating that neutron star mergers play a role in rapid neutron capture (r-process) nucleosynthesis in the universe., (Copyright © 2017, American Association for the Advancement of Science.)

Published
2017
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26. Early spectra of the gravitational wave source GW170817: Evolution of a neutron star merger.

Author

Shappee BJ, Simon JD, Drout MR, Piro AL, Morrell N, Prieto JL, Kasen D, Holoien TW, Kollmeier JA, Kelson DD, Coulter DA, Foley RJ, Kilpatrick CD, Siebert MR, Madore BF, Murguia-Berthier A, Pan YC, Prochaska JX, Ramirez-Ruiz E, Rest A, Adams C, Alatalo K, Bañados E, Baughman J, Bernstein RA, Bitsakis T, Boutsia K, Bravo JR, Di Mille F, Higgs CR, Ji AP, Maravelias G, Marshall JL, Placco VM, Prieto G, and Wan Z

Abstract

On 17 August 2017, Swope Supernova Survey 2017a (SSS17a) was discovered as the optical counterpart of the binary neutron star gravitational wave event GW170817. We report time-series spectroscopy of SSS17a from 11.75 hours until 8.5 days after the merger. Over the first hour of observations, the ejecta rapidly expanded and cooled. Applying blackbody fits to the spectra, we measured the photosphere cooling from [Formula: see text] to [Formula: see text] kelvin, and determined a photospheric velocity of roughly 30% of the speed of light. The spectra of SSS17a began displaying broad features after 1.46 days and evolved qualitatively over each subsequent day, with distinct blue (early-time) and red (late-time) components. The late-time component is consistent with theoretical models of r-process-enriched neutron star ejecta, whereas the blue component requires high-velocity, lanthanide-free material., (Copyright © 2017, American Association for the Advancement of Science.)

Published
2017
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27. Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star.

Author

Arcavi I, Howell DA, Kasen D, Bildsten L, Hosseinzadeh G, McCully C, Wong ZC, Katz SR, Gal-Yam A, Sollerman J, Taddia F, Leloudas G, Fremling C, Nugent PE, Horesh A, Mooley K, Rumsey C, Cenko SB, Graham ML, Perley DA, Nakar E, Shaviv NJ, Bromberg O, Shen KJ, Ofek EO, Cao Y, Wang X, Huang F, Rui L, Zhang T, Li W, Li Z, Zhang J, Valenti S, Guevel D, Shappee B, Kochanek CS, Holoien TW, Filippenko AV, Fender R, Nyholm A, Yaron O, Kasliwal MM, Sullivan M, Blagorodnova N, Walters RS, Lunnan R, Khazov D, Andreoni I, Laher RR, Konidaris N, Wozniak P, and Bue B

Abstract

Every supernova so far observed has been considered to be the terminal explosion of a star. Moreover, all supernovae with absorption lines in their spectra show those lines decreasing in velocity over time, as the ejecta expand and thin, revealing slower-moving material that was previously hidden. In addition, every supernova that exhibits the absorption lines of hydrogen has one main light-curve peak, or a plateau in luminosity, lasting approximately 100 days before declining. Here we report observations of iPTF14hls, an event that has spectra identical to a hydrogen-rich core-collapse supernova, but characteristics that differ extensively from those of known supernovae. The light curve has at least five peaks and remains bright for more than 600 days; the absorption lines show little to no decrease in velocity; and the radius of the line-forming region is more than an order of magnitude bigger than the radius of the photosphere derived from the continuum emission. These characteristics are consistent with a shell of several tens of solar masses ejected by the progenitor star at supernova-level energies a few hundred days before a terminal explosion. Another possible eruption was recorded at the same position in 1954. Multiple energetic pre-supernova eruptions are expected to occur in stars of 95 to 130 solar masses, which experience the pulsational pair instability. That model, however, does not account for the continued presence of hydrogen, or the energetics observed here. Another mechanism for the violent ejection of mass in massive stars may be required.

Published
2017
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28. Astronomy. ASASSN-15lh: A highly super-luminous supernova.

Author

Dong S, Shappee BJ, Prieto JL, Jha SW, Stanek KZ, Holoien TW, Kochanek CS, Thompson TA, Morrell N, Thompson IB, Basu U, Beacom JF, Bersier D, Brimacombe J, Brown JS, Bufano F, Chen P, Conseil E, Danilet AB, Falco E, Grupe D, Kiyota S, Masi G, Nicholls B, Olivares E F, Pignata G, Pojmanski G, Simonian GV, Szczygiel DM, and Woźniak PR

Abstract

We report the discovery of ASASSN-15lh (SN 2015L), which we interpret as the most luminous supernova yet found. At redshift z = 0.2326, ASASSN-15lh reached an absolute magnitude of Mu ,AB = -23.5 ± 0.1 and bolometric luminosity Lbol = (2.2 ± 0.2) × 10(45) ergs s(-1), which is more than twice as luminous as any previously known supernova. It has several major features characteristic of the hydrogen-poor super-luminous supernovae (SLSNe-I), whose energy sources and progenitors are currently poorly understood. In contrast to most previously known SLSNe-I that reside in star-forming dwarf galaxies, ASASSN-15lh appears to be hosted by a luminous galaxy (MK ≈ -25.5) with little star formation. In the 4 months since first detection, ASASSN-15lh radiated (1.1 ± 0.2) × 10(52) ergs, challenging the magnetar model for its engine., (Copyright © 2016, American Association for the Advancement of Science.)

Published
2016
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