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143 results on '"Schultz, A. S. B."'

1. The optical light curve of GRB 221009A: the afterglow and the emerging supernova

Author: Fulton, M. D., Smartt, S. J., Rhodes, L., Huber, M. E., Villar, A. V., Moore, T., Srivastav, S., Schultz, A. S. B., Chambers, K. C., Izzo, L., Hjorth, J., Chen, T. -W., Nicholl, M., Foley, R. J., Rest, A., Smith, K. W., Young, D. R., Sim, S. A., Bright, J., Zenati, Y., de Boer, T., Bulger, J., Fairlamb, J., Gao, H., Lin, C. -C., Lowe, T., Magnier, E. A., Smith, I. A., Wainscoat, R., Coulter, D. A., Jones, D. O., Kilpatrick, C. D., McGill, P., Ramirez-Ruiz, E., Lee, K. -S., Narayan, G., Ramakrishnan, V., Ridden-Harper, R., Singh, A., Wang, Q., Kong, A. K. H., Ngeow, C. -C., Pan, Y. -C., Yang, S., Davis, K. W., Piro, A. L., Rojas-Bravo, C., Sommer, J., and Yadavalli, S. K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present extensive optical photometry of the afterglow of GRB~221009A. Our data cover $0.9 - 59.9$\,days from the time of \textit{Swift} and \textit{Fermi} GRB detections. Photometry in $rizy$-band filters was collected primarily with Pan-STARRS and supplemented by multiple 1- to 4-meter imaging facilities. We analyzed the Swift X-ray data of the afterglow and found a single decline rate power-law $f(t) \propto t^{-1.556\pm0.002}$ best describes the light curve. In addition to the high foreground Milky Way dust extinction along this line of sight, the data favour additional extinction to consistently model the optical to X-ray flux with optically thin synchrotron emission. We fit the X-ray-derived power-law to the optical light curve and find good agreement with the measured data up to $5-6$\,days. Thereafter we find a flux excess in the $riy$ bands which peaks in the observer frame at $\sim20$\,days. This excess shares similar light curve profiles to the type Ic broad-lined supernovae SN~2016jca and SN~2017iuk once corrected for the GRB redshift of $z=0.151$ and arbitrarily scaled. This may be representative of a supernova emerging from the declining afterglow. We measure rest-frame absolute peak AB magnitudes of $M_g=-19.8\pm0.6$ and $M_r=-19.4\pm0.3$ and $M_z=-20.1\pm0.3$. If this is an SN component, then Bayesian modelling of the excess flux would imply explosion parameters of $M_{\rm ej}=7.1^{+2.4}_{-1.7}$ M$_{\odot}$, $M_{\rm Ni}=1.0^{+0.6}_{-0.4}$ M$_{\odot}$, and $v_{\rm ej}=33,900^{+5,900}_{-5,700} kms^{-1}$, for the ejecta mass, nickel mass and ejecta velocity respectively, inferring an explosion energy of $E_{\rm kin}\simeq 2.6-9.0\times10^{52}$ ergs., Comment: Submitted to ApJL on 23rd January 2023, for consideration for publication in the special issue on GRB 221009A. Accepted on 2nd March 2023. The results of this paper are under press embargo until 28th March 2023. 15 pages, 7 figures, 1 table
Published: 2023
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2. The Foundation Supernova Survey: Photospheric Velocity Correlations in Type Ia Supernovae

Author: Dettman, Kyle G., Jha, Saurabh W., Dai, Mi, Foley, Ryan J., Rest, Armin, Scolnic, Daniel M., Siebert, Matthew R., Chambers, K. C., Coulter, D. A., Huber, M. E., Johnson, E., Jones, D. O., Kilpatrick, C. D., Kirshner, R. P., Pan, Y. -C., Riess, A. G., and Schultz, A. S. B.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: The ejecta velocities of type-Ia supernovae (SNe Ia), as measured by the Si II $\lambda 6355$ line, have been shown to correlate with other supernova properties, including color and standardized luminosity. We investigate these results using the Foundation Supernova Survey, with a spectroscopic data release presented here, and photometry analyzed with the SALT2 light-curve fitter. We find that the Foundation data do not show significant evidence for an offset in color between SNe Ia with high and normal photospheric velocities, with $\Delta c = 0.005 \pm 0.014$. Our SALT2 analysis does show evidence for redder high-velocity SN Ia in other samples, including objects from the Carnegie Supernova Project, with a combined sample yielding $\Delta c = 0.017 \pm 0.007$. When split on velocity, the Foundation SN Ia also do not show a significant difference in Hubble diagram residual, $\Delta HR = 0.015 \pm 0.049$ mag. Intriguingly, we find that SN Ia ejecta velocity information may be gleaned from photometry, particularly in redder optical bands. For high-redshift SN Ia, these rest-frame red wavelengths will be observed by the Nancy Grace Roman Space Telescope. Our results also confirm previous work that SN Ia host-galaxy stellar mass is strongly correlated with ejecta velocity: high-velocity SN Ia are found nearly exclusively in high-stellar-mass hosts. However, host-galaxy properties alone do not explain velocity-dependent differences in supernova colors and luminosities across samples. Measuring and understanding the connection between intrinsic explosion properties and supernova environments, across cosmic time, will be important for precision cosmology with SNe Ia., Comment: Submitted to AAS Journals
Published: 2021
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3. Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger S190814bv

Author: Ackley, K., Amati, L., Barbieri, C., Bauer, F. E., Benetti, S., Bernardini, M. G., Bhirombhakdi, K., Botticella, M. T., Branchesi, M., Brocato, E., Bruun, S. H., Bulla, M., Campana, S., Cappellaro, E., Castro-Tirado, A. J., Chambers, K. C., Chaty, S., Chen, T. -W., Ciolfi, R., Coleiro, A., Copperwheat, C. M., Covino, S., Cutter, R., D'Ammando, F., D'Avanzo, P., De Cesare, G., D'Elia, V., Della Valle, M., Denneau, L., De Pasquale, M., Dhillon, V. S., Dyer, M. J., Elias-Rosa, N., Evans, P. A., Eyles-Ferris, R. A. J., Fiore, A., Fraser, M., Fruchter, A. S., Fynbo, J. P. U., Galbany, L., Gall, C., Galloway, D. K., Getman, F. I., Ghirlanda, G., Gillanders, J. H., Gomboc, A., Gompertz, B. P., González-Fernández, C., González-Gaitán, S., Grado, A., Greco, G., Gromadzki, M., Groot, P. J., Gutiérrez, C. P., Heikkilä, T., Heintz, K. E., Hjorth, J., Hu, Y. -D., Huber, M. E., Inserra, C., Izzo, L., Japelj, J., Jerkstrand, A., Jin, Z. P., Jonker, P. G., Kankare, E., Kann, D. A., Kennedy, M., Kim, S., Klose, S., Kool, E. C., Kotak, R., Kuncarayakti, H., Lamb, G. P., Leloudas, G., Levan, A. J., Longo, F., Lowe, T. B., Lyman, J. D., Magnier, E., Maguire, K., Maiorano, E., Mandel, I., Mapelli, M., Mattila, S., McBrien, O. R., Melandri, A., Michałowski, M. J., Milvang-Jensen, B., Moran, S., Nicastro, L., Nicholl, M., Guelbenzu, A. Nicuesa, Nuttal, L., Oates, S. R., O'Brien, P. T., Onori, F., Palazzi, E., Patricelli, B., Perego, A., Torres, M. A. P., Perley, D. A., Pian, E., Pignata, G., Piranomonte, S., Poshyachinda, S., Possenti, A., Pumo, M. L., Quirola-Vásquez, J., Ragosta, F., Ramsay, G., Rau, A., Rest, A., Reynolds, T. M., Rosetti, S. S., Rossi, A., Rosswog, S., Sabha, N. B., Carracedo, A. Sagués, Salafia, O. S., Salmon, L., Salvaterra, R., Savaglio, S., Sbordone, L., Schady, P., Schipani, P., Schultz, A. S. B., Schweyer, T., Smartt, S. J., Smith, K. W., Smith, M., Sollerman, J., Srivastav, S., Stanway, E. R., Starling, R. L. C., Steeghs, D., Stratta, G., Stubbs, C. W., Tanvir, N. R., Testa, V., Thrane, E., Tonry, J. L., Turatto, M., Ulaczyk, K., van der Horst, A. J., Vergani, S. D., Walton, N. A., Watson, D., Wiersema, K., Wiik, K., Wyrzykowski, L., Yang, S., Yi, S. -X., and Young, D. R.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: On 2019 August 14, the LIGO and Virgo interferometers detected a high-significance event labelled S190814bv. Preliminary analysis of the GW data suggests that the event was likely due to the merger of a compact binary system formed by a BH and a NS. ElectromagNetic counterparts of GRAvitational wave sources at the VEry Large Telescope (ENGRAVE) collaboration members carried out an intensive multi-epoch, multi-instrument observational campaign to identify the possible optical/near infrared counterpart of the event. In addition, the ATLAS, GOTO, GRAWITA-VST, Pan-STARRS and VINROUGE projects also carried out a search on this event. Our observations allow us to place limits on the presence of any counterpart and discuss the implications for the kilonova (KN) possibly generated by this NS-BH merger, and for the strategy of future searches. Altogether, our observations allow us to exclude a KN with large ejecta mass $M\gtrsim 0.1\,\mathrm{M_\odot}$ to a high ($>90\%$) confidence, and we can exclude much smaller masses in a subsample of our observations. This disfavours the tidal disruption of the neutron star during the merger. Despite the sensitive instruments involved in the campaign, given the distance of S190814bv we could not reach sufficiently deep limits to constrain a KN comparable in luminosity to AT 2017gfo on a large fraction of the localisation probability. This suggests that future (likely common) events at a few hundreds Mpc will be detected only by large facilities with both high sensitivity and large field of view. Galaxy-targeted observations can reach the needed depth over a relevant portion of the localisation probability with a smaller investment of resources, but the number of galaxies to be targeted in order to get a fairly complete coverage is large, even in the case of a localisation as good as that of this event., Comment: 52 pages, revised version now accepted for publication in A&A. Abstract abridged to meet arXiv requirements
Published: 2020
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4. Searching for Super-Fast Rotators Using the Pan-STARRS 1

Author: Chang, Chan-Kao, Lin, Hsing-Wen, Ip, Wing-Huen, Chen, Wen-Ping, Yeh, Ting-Shuo, Chambers, K. C., Magnier, E. A., Huber, M. E., Flewelling, H. A., Waters, C. Z., Wainscoat, R. J., and Schultz, A. S. B.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: A class of asteroids, called large super-fast rotators (large SFRs), have rotation periods shorter than 2 hours and diameters larger than ~ 0.3 km. They pose challenges to the usual interior rubble-pile structure unless a relatively high bulk density is assumed. So far, only six large SFRs have been found. Therefore, we present a survey of asteroid rotation period using Pan-STARRS 1 telescopes during 2016 October 26 to 31 to search more large SFRs and study their properties. A total of 876 reliable rotation periods are measured, among which seven are large SFRs, thereby increasing the inventory of known large SFRs. These seven newly discovered large SFRs have diverse colors and locations in the main asteroid belt, suggesting that the taxonomic tendency and the location preference in the inner main belt of the six perviously known large SFRs could be a bias due to various observational limits. Interestingly, five out of the seven newly discovered large SFRs are mid main-belt asteroids. Considering the rare discovery rates of large SFR in the previously similar surveys (Chang et al., 2015, 2016) and the survey condition in this work, the chance of detecting a large SFR in the inner main belt seems to be relatively low. This probably suggests that the inner main belt harbors less large SFRs than the mid main belt. From our survey, we also found the drop in number appearing at f > 5 rev/day on the spin-rate distribution for the outer main-belt asteroids of D < 3 km, which was reported for the inner and mid main belt by (Chang et al., 2015, 2016)., Comment: Accepted by ApJS on Jan 24, 2019
Published: 2019
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5. K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova

Author: Dimitriadis, G., Foley, R. J., Rest, A., Kasen, D., Piro, A. L., Polin, A., Jones, D. O., Villar, A., Narayan, G., Coulter, D. A., Kilpatrick, C. D., Pan, Y. -C., Rojas-Bravo, C., Fox, O. D., Jha, S. W., Nugent, P. E., Riess, A. G., Scolnic, D., Drout, M. R., Barentsen, G., Dotson, J., Gully-Santiago, M., Hedges, C., Cody, A. M., Barclay, T., Howell, S., Garnavich, P., Tucker, B. E., Shaya, E., Mushotzky, R., Olling, R. P., Margheim, S., Zenteno, A., Coughlin, J., Van Cleve, J. E., Cardoso, J. Vinicius de Miranda, Larson, K. A., McCalmont-Everton, K. M., Peterson, C. A., Ross, S. E., Reedy, L. H., Osborne, D., McGinn, C., Kohnert, L., Migliorini, L., Wheaton, A., Spencer, B., Labonde, C., Castillo, G., Beerman, G., Steward, K., Hanley, M., Larsen, R., Gangopadhyay, R., Kloetzel, R., Weschler, T., Nystrom, V., Moffatt, J., Redick, M., Griest, K., Packard, M., Muszynski, M., Kampmeier, J., Bjella, R., Flynn, S., Elsaesser, B., Chambers, K. C., Flewelling, H. A., Huber, M. E., Magnier, E. A., Waters, C. Z., Schultz, A. S. B., Bulger, J., Lowe, T. B., Willman, M., Smartt, S. J., Smith, K. W., Points, S., Strampelli, G. M., Brimacombe, J., Chen, P., Munoz, J. A., Mutel, R. L., Shields, J., Vallely, P. J., Villanueva Jr, S., Li, W., Wang, X., Zhang, J., Lin, H., Mo, J., Zhao, X., Sai, H., Zhang, X., Zhang, K., Zhang, T., Wang, L., Baron, E., DerKacy, J. M., Li, L., Chen, Z., Xiang, D., Rui, L., Huang, F., Li, X., Hosseinzadeh, G., Howell, D. A., Arcavi, I., Hiramatsu, D., Burke, J., Valenti, S., Tonry, J. L., Denneau, L., Heinze, A. N., Weiland, H., Stalder, B., Vinko, J., Sarneczky, K., Pa, A., Bodi, A., Bognar, Zs., Csak, B., Cseh, B., Csornyei, G., Hanyecz, O., Ignacz, B., Kalup, Cs., Konyves-Toth, R., Kriskovics, L., Ordasi, A., Rajmon, I., Sodor, A., Szabo, R., Szakats, R., Zsidi, G., Williams, S. C., Nordin, J., Cartier, R., Frohmaier, C., Galbany, L., Gutierrez, C. P., Hook, I., Inserra, C., Smith, M., Sand, D. J., Andrews, J. E., Smith, N., and Bilinski, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present an exquisite, 30-min cadence Kepler (K2) light curve of the Type Ia supernova (SN Ia) 2018oh (ASASSN-18bt), starting weeks before explosion, covering the moment of explosion and the subsequent rise, and continuing past peak brightness. These data are supplemented by multi-color Pan-STARRS1 and CTIO 4-m DECam observations obtained within hours of explosion. The K2 light curve has an unusual two-component shape, where the flux rises with a steep linear gradient for the first few days, followed by a quadratic rise as seen for typical SNe Ia. This "flux excess" relative to canonical SN Ia behavior is confirmed in our $i$-band light curve, and furthermore, SN 2018oh is especially blue during the early epochs. The flux excess peaks 2.14$\pm0.04$ days after explosion, has a FWHM of 3.12$\pm0.04$ days, a blackbody temperature of $T=17,500^{+11,500}_{-9,000}$ K, a peak luminosity of $4.3\pm0.2\times10^{37}\,{\rm erg\,s^{-1}}$, and a total integrated energy of $1.27\pm0.01\times10^{43}\,{\rm erg}$. We compare SN 2018oh to several models that may provide additional heating at early times, including collision with a companion and a shallow concentration of radioactive nickel. While all of these models generally reproduce the early K2 light curve shape, we slightly favor a companion interaction, at a distance of $\sim$$2\times10^{12}\,{\rm cm}$ based on our early color measurements, although the exact distance depends on the uncertain viewing angle. Additional confirmation of a companion interaction in future modeling and observations of SN 2018oh would provide strong support for a single-degenerate progenitor system., Comment: 20 pages, 9 figures, 2 tables. Submitted to APJ Letters on 31 Jul 2018, Accepted for publication on 31 Aug 2018
Published: 2018
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6. Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the $Kepler$ 2 Observations

Author: Li, W., Wang, X., Vinkó, J., Mo, J., Hosseinzadeh, G., Sand, D. J., Zhang, J., Lin, H., Zhang, T., Wang, L., Chen, Z., Xiang, D., Rui, L., Huang, F., Li, X., Zhang, X., Li, L., Baron, E., Derkacy, J. M., Zhao, X., Sai, H., Zhang, K., Howell, D. A., McCully, C., Arcavi, I., Valenti, S., Hiramatsu, D., Burke, J., Rest, A., Garnavich, P., Tucker, B. E., Narayan, G., Shaya, E., Margheim, S., Zenteno, A., Villar, A., Dimitriadis, G., Foley, R. J., Pan, Y. -C., Coulter, D. A., Fox, O. D., Jha, S. W., Jones, D. O., Kasen, D. N., Kilpatrick, C. D., Piro, A. L., Riess, A. G., Rojas-Bravo, C., Shappee, B. J., Holoien, T. W. -S., Stanek, K. Z., Drout, M. R., Auchettl, K., Kochanek, C. S., Brown, J. S., Bose, S., Bersier, D., Brimacombe, J., Chen, P., Dong, S., Holmbo, S., Muñoz, J. A., Mutel, R. L., Post, R. S., Prieto, J. L., Shields, J., Tallon, D., Thompson, T. A., Vallely, P. J., Villanueva Jr., S., Smartt, S. J., Smith, K. W., Chambers, K. C., Flewelling, H. A., Huber, M. E., Magnier, E. A., Waters, C. Z., Schultz, A. S. B., Bulger, J., Lowe, T. B., Willman, M., Sárneczky, K., Pál, A., Wheeler, J. C., Bódi, A., Bognár, Zs., Csák, B., Cseh, B., Csörnyei, G., Hanyecz, O., Ignácz, B., Kalup, Cs., Könyves-Tóth, R., Kriskovics, L., Ordasi, A., Rajmon, I., Sódor, A., Szabó, R., Szakáts, R., Zsidi, G., Milne, P., Andrews, J. E., Smith, N., Bilinski, C., Brown, P. J., Nordin, J., Williams, S. C., Galbany, L., Palmerio, J., Hook, I. M., Inserra, C., Maguire, K., Cartier, Régis, Razza, A., Gutiérrez, C. P., Hermes, J. J., Reding, J. S., Kaiser, B. C., Tonry, J. L., Heinze, A. N., Denneau, L., Weiland, H., Stalder, B., Barentsen, G., Dotson, J., Barclay, T., Gully-Santiago, M., Hedges, C., Cody, A. M., Howell, S., Coughlin, J., Van Cleve, J. E., Cardoso, J. Vinícius de Miranda, Larson, K. A., McCalmont-Everton, K. M., Peterson, C. A., Ross, S. E., Reedy, L. H., Osborne, D., McGinn, C., Kohnert, L., Migliorini, L., Wheaton, A., Spencer, B., Labonde, C., Castillo, G., Beerman, G., Steward, K., Hanley, M., Larsen, R., Gangopadhyay, R., Kloetzel, R., Weschler, T., Nystrom, V., Moffatt, J., Redick, M., Griest, K., Packard, M., Muszynski, M., Kampmeier, J., Bjella, R., Flynn, S., and Elsaesser, B.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically-confirmed type Ia supernova (SN Ia) observed in the $Kepler$ field. The $Kepler$ data revealed an excess emission in its early light curve, allowing to place interesting constraints on its progenitor system (Dimitriadis et al. 2018, Shappee et al. 2018b). Here, we present extensive optical, ultraviolet, and near-infrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3$\pm$0.3 days and $\Delta$m$_{15}(B)=0.96\pm$0.03 mag, but it seems to have bluer $B - V$ colors. We construct the "uvoir" bolometric light curve having peak luminosity as 1.49$\times$10$^{43}$erg s$^{-1}$, from which we derive a nickel mass as 0.55$\pm$0.04M$_{\odot}$ by fitting radiation diffusion models powered by centrally located $^{56}$Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of $^{56}$Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a non-degenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia, but is characterized by prominent and persistent carbon absorption features. The C II features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in a SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers., Comment: 48 pages, 23 figures. This paper is part of a coordinated effort between groups. Accepted for publication in ApJ
Published: 2018
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7. The Foundation Supernova Survey: Measuring Cosmological Parameters with Supernovae from a Single Telescope

Author: Jones, D. O., Scolnic, D. M., Foley, R. J., Rest, A., Kessler, R., Challis, P. M., Chambers, K. C., Coulter, D. A., Dettman, K. G., Foley, M. M., Huber, M. E., Jha, S. W., Johnson, E., Kilpatrick, C. D., Kirshner, R. P., Manuel, J., Narayan, G., Pan, Y. -C., Riess, A. G., Schultz, A. S. B., Siebert, M. R., Berger, E., Chornock, R., Flewelling, H., Magnier, E. A., Smartt, S. J., Smith, K. W., Wainscoat, R. J., Waters, C., and Willman, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Measurements of the dark energy equation-of-state parameter, $w$, have been limited by uncertainty in the selection effects and photometric calibration of $z<0.1$ Type Ia supernovae (SNe Ia). The Foundation Supernova Survey is designed to lower these uncertainties by creating a new sample of $z<0.1$ SNe Ia observed on the Pan-STARRS system. Here, we combine the Foundation sample with SNe from the Pan-STARRS Medium Deep Survey and measure cosmological parameters with 1,338 SNe from a single telescope and a single, well-calibrated photometric system. For the first time, both the low-$z$ and high-$z$ data are predominantly discovered by surveys that do not target pre-selected galaxies, reducing selection bias uncertainties. The $z>0.1$ data include 875 SNe without spectroscopic classifications and we show that we can robustly marginalize over CC SN contamination. We measure Foundation Hubble residuals to be fainter than the pre-existing low-$z$ Hubble residuals by $0.046 \pm 0.027$ mag (stat+sys). By combining the SN Ia data with cosmic microwave background constraints, we find $w=-0.938 \pm 0.053$, consistent with $\Lambda$CDM. With 463 spectroscopically classified SNe Ia alone, we measure $w=-0.933\pm0.061$. Using the more homogeneous and better-characterized Foundation sample gives a 55% reduction in the systematic uncertainty attributed to SN Ia sample selection biases. Although use of just a single photometric system at low and high redshift increases the impact of photometric calibration uncertainties in this analysis, previous low-$z$ samples may have correlated calibration uncertainties that were neglected in past studies. The full Foundation sample will observe up to 800 SNe to anchor the LSST and WFIRST Hubble diagrams., Comment: 30 pages, 17 figures, accepted by ApJ
Published: 2018
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8. PS18kh: A New Tidal Disruption Event with a Non-Axisymmetric Accretion Disk

Author: Holoien, T. W. -S., Huber, M. E., Shappee, B. J., Eracleous, M., Auchettl, K., Brown, J. S., Tucker, M. A., Chambers, K. C., Kochanek, C. S., Stanek, K. Z., Rest, A., Bersier, D., Post, R. S., Aldering, G., Ponder, K. A., Simon, J. D., Kankare, E., Dong., D., Hallinan, G., Reddy, N. A., Sanders, R. L., Topping, M. W., Bulger, J., Lowe, T. B., Magnier, E. A., Schultz, A. S. B., Waters, C. Z., Willman, M., Wright, D., Young, D. R., Dong, Subo, Prieto, J. L., Thompson, Todd A., Denneau, L., Flewelling, H., Heinze, A. N., Smartt, S. J., Smith, K. W., Stalder, B., Tonry, J. L., and Weiland, H.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the discovery of PS18kh, a tidal disruption event (TDE) discovered at the center of SDSS J075654.53+341543.6 ($d\simeq322$ Mpc) by the Pan-STARRS Survey for Transients. Our dataset includes pre-discovery survey data from Pan-STARRS, the All-Sky Automated Survey for Supernovae (ASAS-SN), and the Asteroid Terrestrial-impact Last Alert System (ATLAS) as well as high-cadence, multi-wavelength 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 $T\simeq12000$ K to $T\simeq25000$ K and it peaked at a luminosity of $L\simeq8.8\times10^{43}$ ergs s$^{-1}$. PS18kh radiated $E=(3.45\pm0.22)\times10^{50}$ ergs over the period of observation, with $(1.42\pm0.20)\times10^{50}$ ergs being released during the rise to peak. Spectra of PS18kh show a changing, boxy/double-peaked H$\alpha$ emission feature, which becomes more prominent over time. We use models of non-axisymmetric accretion disks to describe the profile of the H$\alpha$ 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 $r_{\rm in}\sim60r_{\rm g}$ to an outer radius of $r_{\rm out}\sim1400r_{\rm g}$ 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., Comment: 27 pages, 13 figures, 8 tables. Updated to reflect changes made in the published version. A table containing the host-subtracted photometry presented in this manuscript is included in machine-readable format as an ancillary file
Published: 2018
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9. Seeing Double: ASASSN-18bt Exhibits a Two-Component Rise in the Early-Time K2 Light Curve

Author: Shappee, B. J., Holoien, T. W. -s., Drout, M. R., Auchettl, K., Stritzinger, M. D., Kochanek, C. S., Stanek, K. Z., Shaya, E., Narayan, G., Brown, J. S., Bose, S., Bersier, D., Brimacombe, J., Chen, Ping, Dong, Subo, Holmbo, S., Katz, B., Munnoz, J. A., Mutel, R. L., Post, R. S., Prieto, J. L., Shields, J., Tallon, D., Thompson, T. A., Vallely, P. J., Villanueva Jr., S., Denneau, L., Flewelling, H., Heinze, A. N., Smith, K. W., Stalder, B., Tonry, J. L., Weiland, H., Barclay, T., Barentsen, G., Cody, A. M., Dotson, J., Foerster, F., Garnavich, P., Gully-santiago, M., Hedges, C., Howell, S., Kasen, D., Margheim, S., Mushotzky, R., Rest, A., Tucker, B. E., 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, K. A., Mccalmont-everton, K. M., Mcginn, C., Migliorini, L., Moffatt, J., Muszynski, M., Nystrom, V., Osborne, D., Packard, M., Peterson, C. A., Redick, M., Reedy, L. H., Ross, S. E., Spencer, B., Steward, K., Van Cleve, J. E., Cardoso, J. Vinicius De Miranda, Weschler, T., Wheaton, A., Bulger, J., Lowe, T. B., Magnier, E. A., Schultz, A. S. B., Waters, C. Z., Willman, M., Baron, Eddie, Chen, Zhihao, Derkacy, James M., Huang, Fang, Li, Linyi, Li, Wenxiong, Li, Xue, Rui, Liming, Sai, Hanna, Wang, Lifan, Wang, Lingzhi, Wang, Xiaofeng, Xiang, Danfeng, Zhang, Jicheng, Zhang, Jujia, Zhang, Kaicheng, Zhang, Tianmeng, Zhang, Xinghan, Zhao, Xulin, Brown, P. J., Hermes, J. J., Nordin, J., Points, S., and Strampelli, G. M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
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<4.5 * 10^5 cm^-3 at a radius of 4 *10^15 cm from the progenitor star. Assuming a wind-like environment, we place mass-loss limits of Mdot< 8 * 10^-6 M_sun yr^-1 for v_w=100 km s^-1, ruling out some symbiotic progenitor systems., Comment: 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: 2018
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10. Should Type Ia Supernova Distances be Corrected for their Local Environments?

Author: Jones, D. O., Riess, A. G., Scolnic, D. M., Pan, Y. -C., Johnson, E., Coulter, D. A., Dettman, K. G., Foley, M. M., Foley, R. J., Huber, M. E., Jha, S. W., Kilpatrick, C. D., Kirshner, R. P., Rest, A., Schultz, A. S. B., and Siebert, M. R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Recent analyses suggest that distance residuals measured from Type Ia supernovae (SNe Ia) are correlated with local host galaxy properties within a few kpc of the SN explosion. However, the well-established correlation with global host galaxy properties is nearly as significant, with a shift of 0.06 mag across a low to high mass boundary (the mass step). Here, with 273 SNe Ia at $z<0.1$, we investigate whether stellar masses and rest-frame $u-g$ colors of regions within 1.5 kpc of the SN Ia explosion site are significantly better correlated with SN distance measurements than global properties or properties measured at random locations in SN hosts. At $\lesssim2\sigma$ significance, local properties tend to correlate with distance residuals better than properties at random locations, though despite using the largest low-$z$ sample to date we cannot definitively prove that a local correlation is more significant than a random correlation. Our data hint that SNe observed by surveys that do not target a pre-selected set of galaxies may have a larger local mass step than SNe from surveys that do, an increase of $0.071\pm0.036$ mag (2.0$\sigma$). We find a $3\sigma$ local mass step after global mass correction, evidence that SNe Ia should be corrected for their local mass, but we note that this effect is insignificant in the targeted low-$z$ sample. Only the local mass step remains significant at $>2\sigma$ after global mass correction, and we conservatively estimate a systematic shift in H$_0$ measurements of -0.14 $\textrm{km}\,\textrm{s}^{-1}\textrm{Mpc}^{-1}$ with an additional uncertainty of 0.14 $\textrm{km}\,\textrm{s}^{-1}\textrm{Mpc}^{-1}$, $\sim$10\% of the present uncertainty., Comment: Accepted for publication in ApJ
Published: 2018
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11. The Foundation Supernova Survey: Motivation, Design, Implementation, and First Data Release

Author: Foley, Ryan J., Scolnic, Daniel, Rest, Armin, Jha, S. W., Pan, Y. -C., Riess, A. G., Challis, P., Chambers, K. C., Coulter, D. A., Dettman, K. G., Foley, M. M., Fox, O. D., Huber, M. E., Jones, D. O., Kilpatrick, C. D., Kirshner, R. P., Schultz, A. S. B., Siebert, M. R., Flewelling, H. A., Gibson, B., Magnier, E. A., Miller, J. A., Primak, N., Smartt, S. J., Smith, K. W., Wainscoat, R. J., Waters, C., and Willman, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Foundation Supernova Survey aims to provide a large, high-fidelity, homogeneous, and precisely-calibrated low-redshift Type Ia supernova (SN Ia) sample for cosmology. The calibration of the current low-redshift SN sample is the largest component of systematic uncertainties for SN cosmology, and new data are necessary to make progress. We present the motivation, survey design, observation strategy, implementation, and first results for the Foundation Supernova Survey. We are using the Pan-STARRS telescope to obtain photometry for up to 800 SNe Ia at z < 0.1. This strategy has several unique advantages: (1) the Pan-STARRS system is a superbly calibrated telescopic system, (2) Pan-STARRS has observed 3/4 of the sky in grizy making future template observations unnecessary, (3) we have a well-tested data-reduction pipeline, and (4) we have observed ~3000 high-redshift SNe Ia on this system. Here we present our initial sample of 225 SN Ia griz light curves, of which 180 pass all criteria for inclusion in a cosmological sample. The Foundation Supernova Survey already contains more cosmologically useful SNe Ia than all other published low-redshift SN Ia samples combined. We expect that the systematic uncertainties for the Foundation Supernova Sample will be 2-3 times smaller than other low-redshift samples. We find that our cosmologically useful sample has an intrinsic scatter of 0.111 mag, smaller than other low-redshift samples. We perform detailed simulations showing that simply replacing the current low-redshift SN Ia sample with an equally sized Foundation sample will improve the precision on the dark energy equation-of-state parameter by 35%, and the dark energy figure-of-merit by 72%., Comment: MNRAS, accepted; 157 pages, but 139 pages are tables; 9 figures
Published: 2017
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12. A kilonova as the electromagnetic counterpart to a gravitational-wave source

Author: Smartt, S. J., Chen, T. -W., Jerkstrand, A., Coughlin, M., Kankare, E., Sim, S. A., Fraser, M., Inserra, C., Maguire, K., Chambers, K. C., Huber, M. E., Kruhler, T., Leloudas, G., Magee, M., Shingles, L. J., Smith, K. W., Young, D. R., Tonry, J., Kotak, R., Gal-Yam, A., Lyman, J. D., Homan, D. S., Agliozzo, C., Anderson, J. P., Ashall, C. R. Angus C., Barbarino, C., Bauer, F. E., Berton, M., Botticella, M. T., Bulla, M., Bulger, J., Cannizzaro, G., Cano, Z., Cartier, R., Cikota, A., Clark, P., De Cia, A., Della Valle, M., Denneau, L., Dennefeld, M., Dessart, L., Dimitriadis, G., Elias-Rosa, N., Firth, R. E., Flewelling, H., Flors, A., Franckowiak, A., Frohmaier, C., Galbany, L., Gonzalez-Gaitan, S., Greiner, J., Gromadzki, M., Guelbenzu, A. Nicuesa, Gutierrez, C. P., Hamanowicz, A., Hanlon, L., Harmanen, J., Heintz, K. E., Heinze, A., Hernandez, M. -S., Hodgkin, S. T., Hook, I. M., Izzo, L., James, P. A., Jonker, P. G., Kerzendorf, W. E., Klose, S., Kostrzewa-Rutkowska, Z., Kowalski, M., Kromer, M., Kuncarayakti, H., Lawrence, A., Lowe, T. B., Magnier, E. A., Manulis, I., Martin-Carrillo, A., Mattila, S., McBrien, O., Muller, A., Nordin, J., O'Neill, D., Onori, F., Palmerio, J. T., Pastorello, A., Patat, F., Pignata, G., Podsiadlowski, Ph., Pumo, M. L., Prentice, S. J., Rau, A., Razza, A., Rest, A., Reynolds, T., Roy, R., Ruiter, A. J., Rybicki, K. A., Salmon, L., Schady, P., Schultz, A. S. B., Schweyer, T., Seitenzahl, I. R., Smith, M., Sollerman, J., Stalder, B., Stubbs, C. W., Sullivan, M., Szegedi, H., Taddia, F., Taubenberger, S., Terreran, G., van Soelen, B., Vos, J., Wainscoat, R. J., Walton, N. A., Waters, C., Weiland, H., Willman, M., Wiseman, P., Wright, D. E., Wyrzykowski, L., and Yaron, O.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Gravitational waves were discovered with the detection of binary black hole mergers and they should also be detectable from lower mass neutron star mergers. These are predicted to eject material rich in heavy radioactive isotopes that can power an electromagnetic signal called a kilonova. The gravitational wave source GW170817 arose from a binary neutron star merger in the nearby Universe with a relatively well confined sky position and distance estimate. Here we report observations and physical modelling of a rapidly fading electromagnetic transient in the galaxy NGC4993, which is spatially coincident with GW170817 and a weak short gamma-ray burst. The transient has physical parameters broadly matching the theoretical predictions of blue kilonovae from neutron star mergers. The emitted electromagnetic radiation can be explained with an ejected mass of 0.04 +/- 0.01 Msol, with an opacity of kappa <= 0.5 cm2/gm at a velocity of 0.2 +/- 0.1c. The power source is constrained to have a power law slope of beta = -1.2 +/- 0.3, consistent with radioactive powering from r-process nuclides. We identify line features in the spectra that are consistent with light r-process elements (90 < A < 140). As it fades, the transient rapidly becomes red, and emission may have contribution by a higher opacity, lanthanide-rich ejecta component. This indicates that neutron star mergers produce gravitational waves, radioactively powered kilonovae, and are a nucleosynthetic source of the r-process elements., Comment: Nature, in press, DOI 10.1038/nature24303. Data files will be made available at http://www.pessto.org
Published: 2017
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13. Observations of the GRB afterglow ATLAS17aeu and its possible association with GW170104

Author: Stalder, B., Tonry, J., Smartt, S. J., Coughlin, M., Chambers, K. C., Stubbs, C. W., Chen, T. -W., Kankare, E., Smith, K. W., Denneau, L., Sherstyuk, A., Heinze, A., Weiland, H., Rest, A., Young, D. R., Huber, M. E., Flewelling, H., Lowe, T., Magnier, E. A., Schultz, A. S. B., Waters, C., Wainscoat, R., Willman, M., Wright, D. E., Chu, J. K., Sanders, D., Inserra, C., Maguire, K., and Kotak, R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the discovery and multi-wavelength data analysis of the peculiar optical transient, ATLAS17aeu. This transient was identified in the skymap of the LIGO gravitational wave event GW170104 by our ATLAS and Pan-STARRS coverage. ATLAS17aeu was discovered 23.1hrs after GW170104 and rapidly faded over the next 3 nights, with a spectrum revealing a blue featureless continuum. The transient was also detected as a fading x-ray source by Swift and in the radio at 6 and 15 GHz. A gamma ray burst GRB170105A was detected by 3 satellites 19.04hrs after GW170104 and 4.10hrs before our first optical detection. We analyse the multi-wavelength fluxes in the context of the known GRB population and discuss the observed sky rates of GRBs and their afterglows. We find it statistically likely that ATLAS17aeu is an afterglow associated with GRB170105A, with a chance coincidence ruled out at the 99\% confidence or 2.6$\sigma$. A long, soft GRB within a redshift range of $1 \lesssim z \lesssim 2.9$ would be consistent with all the observed multi-wavelength data. The Poisson probability of a chance occurrence of GW170104 and ATLAS17aeu is $p=0.04$. This is the probability of a chance coincidence in 2D sky location and in time. These observations indicate that ATLAS17aeu is plausibly a normal GRB afterglow at significantly higher redshift than the distance constraint for GW170104 and therefore a chance coincidence. However if a redshift of the faint host were to place it within the GW170104 distance range, then physical association with GW170104 should be considered., Comment: 16 pages, 6 figures, accepted to ApJ
Published: 2017
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14. The Pan-STARRS1 Surveys

Author: Chambers, K. C., Magnier, E. A., Metcalfe, N., Flewelling, H. A., Huber, M. E., Waters, C. Z., Denneau, L., Draper, P. W., Farrow, D., Finkbeiner, D. P., Holmberg, C., Koppenhoefer, J., Price, P. A., Rest, A., Saglia, R. P., Schlafly, E. F., Smartt, S. J., Sweeney, W., Wainscoat, R. J., Burgett, W. S., Chastel, S., Grav, T., Heasley, J. N., Hodapp, K. W., Jedicke, R., Kaiser, N., Kudritzki, R. -P., Luppino, G. A., Lupton, R. H., Monet, D. G., Morgan, J. S., Onaka, P. M., Shiao, B., Stubbs, C. W., Tonry, J. L., White, R., Bañados, E., Bell, E. F., Bender, R., Bernard, E. J., Boegner, M., Boffi, F., Botticella, M. T., Calamida, A., Casertano, S., Chen, W. -P., Chen, X., Cole, S., Deacon, N., Frenk, C., Fitzsimmons, A., Gezari, S., Gibbs, V., Goessl, C., Goggia, T., Gourgue, R., Goldman, B., Grant, P., Grebel, E. K., Hambly, N. C., Hasinger, G., Heavens, A. F., Heckman, T. M., Henderson, R., Henning, T., Holman, M., Hopp, U., Ip, W. -H., Isani, S., Jackson, M., Keyes, C. D., Koekemoer, A. M., Kotak, R., Le, D., Liska, D., Long, K. S., Lucey, J. R., Liu, M., Martin, N. F., Masci, G., McLean, B., Mindel, E., Misra, P., Morganson, E., Murphy, D. N. A., Obaika, A., Narayan, G., Nieto-Santisteban, M. A., Norberg, P., Peacock, J. A., Pier, E. A., Postman, M., Primak, N., Rae, C., Rai, A., Riess, A., Riffeser, A., Rix, H. W., Röser, S., Russel, R., Rutz, L., Schilbach, E., Schultz, A. S. B., Scolnic, D., Strolger, L., Szalay, A., Seitz, S., Small, E., Smith, K. W., Soderblom, D. R., Taylor, P., Thomson, R., Taylor, A. N., Thakar, A. R., Thiel, J., Thilker, D., Unger, D., Urata, Y., Valenti, J., Wagner, J., Walder, T., Walter, F., Watters, S. P., Werner, S., Wood-Vasey, W. M., and Wyse, R.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: Pan-STARRS1 has carried out a set of distinct synoptic imaging sky surveys including the $3\pi$ Steradian Survey and the Medium Deep Survey in 5 bands ($grizy_{P1}$). The mean 5$\sigma$ point source limiting sensitivities in the stacked 3$\pi$ Steradian Survey in $grizy_{P1}$ are (23.3, 23.2, 23.1, 22.3, 21.4) respectively. The upper bound on the systematic uncertainty in the photometric calibration across the sky is 7-12 millimag depending on the bandpass. The systematic uncertainty of the astrometric calibration using the Gaia frame comes from a comparison of the results with Gaia: the standard deviation of the mean and median residuals ($ \Delta ra, \Delta dec $) are (2.3, 1.7) milliarcsec, and (3.1, 4.8) milliarcsec respectively. The Pan-STARRS system and the design of the PS1 surveys are described and an overview of the resulting image and catalog data products and their basic characteristics are described together with a summary of important results. The images, reduced data products, and derived data products from the Pan-STARRS1 surveys are available to the community from the Mikulski Archive for Space Telescopes (MAST) at STScI., Comment: 38 pages, 29 figures, 12 tables
Published: 2016

15. A search for an optical counterpart to the gravitational wave event GW151226

Author: Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Chen, T. -W., Inserra, C., Wright, D. E., Coughlin, M., Denneau, L., Flewelling, H., Heinze, A., Jerkstrand, A., Magnier, E. A., Maguire, K., Mueller, B., Rest, A., Sherstyuk, A., Stalder, B., Schultz, A. S. B., Stubbs, C. W., Tonry, J., Waters, C., Wainscoat, R., Della Valle, M., Dennefeld, M., Dimitriadis, G., Firth, R. E., Fraser, M., Frohmaier, C., Gal-Yam, A., Harmanen, J., Kankare, E., Kotak, R., Kromer, M., Mandel, I., Sollerman, J., Gibson, B., Primak, N., and Willman, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present a search for an electromagnetic counterpart of the gravitational wave source GW151226. Using the Pan-STARRS1 telescope we mapped out 290 square degrees in the optical i_ps filter starting 11.5hr after the LIGO information release and lasting for a further 28 days. The first observations started 49.5hr after the time of the GW151226 detection. We typically reached sensitivity limits of i_ps = 20.3-20.8 and covered 26.5% of the LIGO probability skymap. We supplemented this with ATLAS survey data, reaching 31% of the probability region to shallower depths of m~19. We found 49 extragalactic transients (that are not obviously AGN), including a faint transient in a galaxy at 7Mpc (a luminous blue variable outburst) plus a rapidly decaying M-dwarf flare. Spectral classification of 20 other transient events showed them all to be supernovae. We found an unusual transient, PS15dpn, with an explosion date temporally coincident with GW151226 which evolved into a type Ibn supernova. The redshift of the transient is secure at z=0.1747 +/- 0.0001 and we find it unlikely to be linked, since the luminosity distance has a negligible probability of being consistent with that of GW151226. In the 290 square degrees surveyed we therefore do not find a likely counterpart. However we show that our survey strategy would be sensitive to NS-NS mergers producing kilonovae at D < 100 Mpc which is promising for future LIGO/Virgo searches., Comment: Submitted to ApJL on 6th June 2016. Accepted on 8th August 2016. This is the accepted version after referee report and minor revisions
Published: 2016
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16. Pan-STARRS and PESSTO search for an optical counterpart to the LIGO gravitational wave source GW150914

Author: Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Cappellaro, E., Wright, D. E., Coughlin, M., Schultz, A. S. B., Denneau, L., Flewelling, H., Heinze, A., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., Anderson, J. P., Baltay, C., Botticella, M. T., Campbell, H., Dennefeld, M., Chen, T. -W., Della Valle, M., Elias-Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kotak, R., Kupfer, T., Harmanen, J., Galbany, L., Gal-Yam, A., Guillou, L. Le, Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Olivares, F. E, Rabinowitz, D., Razza, A., Sollerman, J., Smith, M., Terreran, G., Valenti, S., Gibson, B., and Goggia, T.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We searched for an optical counterpart to the first gravitational wave source discovered by LIGO (GW150914), using a combination of the Pan-STARRS1 wide-field telescope and the PESSTO spectroscopic follow-up programme. As the final LIGO sky maps changed during analysis, the total probability of the source being spatially coincident with our fields was finally only 4.2 per cent. Therefore we discuss our results primarily as a demonstration of the survey capability of Pan-STARRS and spectroscopic capability of PESSTO. We mapped out 442 square degrees of the northern sky region of the initial map. We discovered 56 astrophysical transients over a period of 41 days from the discovery of the source. Of these, 19 were spectroscopically classified and a further 13 have host galaxy redshifts. All transients appear to be fairly normal supernovae and AGN variability and none is obviously linked with GW150914. We illustrate the sensitivity of our survey by defining parameterised lightcurves with timescales of 4, 20 and 40 days and use the sensitivity of the Pan-STARRS1 images to set limits on the luminosities of possible sources. The Pan-STARRS1 images reach limiting magnitudes of i = 19.2, 20.0 and 20.8 respectively for the three timescales. For long timescale parameterised lightcurves (with FWHM=~40d) we set upper limits of M_i <= -17.2 -0.9/+1.4 if the distance to GW150914 is D = 400 +/- 200Mpc. The number of type Ia SN we find in the survey is similar to that expected from the cosmic SN rate, indicating a reasonably complete efficiency in recovering supernova like transients out to D = 400 +/- 200 Mpc., Comment: Accepted for publication on 28 July 2016 in MNRAS.This is the accepted version after referee report and editor acceptance
Published: 2016
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17. NICMOS Observations of Shocked H_2 in Orion

Author: Colgan, Sean W. J., Schultz, A. S. B., Kaufman, M. J., Erickson, E. F., and Hollenbach, D. J.
Subjects: Astrophysics
Abstract: HST NICMOS narrowband images of the shocked molecular hydrogen emission in OMC-1 are analyzed to reveal new information on the BN/KL outflow. The outstanding morphological feature of this region is the array of molecular hydrogen ``fingers'' emanating from the general vicinity of IRc2 and the presence of several Herbig-Haro objects. The NICMOS images appear to resolve individual shock fronts. This work is a more quantitative and detailed analysis of our data from a previous paper (Schultz etal. 1999). Line strengths for the H_2 1--0 S(4) plus 2--1 S(6) lines at 1.89 micron are estimated from measurements with the Paschen_alpha continuum filter F190N at 1.90 micron, and continuum measurements at 1.66 and 2.15 micron. We compare the observed H_2 line strengths and ratios of the 1.89 micron and 2.12 micron 1--0 S(1) lines with models for molecular cloud shock waves. Most of the data cannot be fit by J-shocks, but are well matched by C-shocks with shock velocities in the range of 20--45 km/s and preshock densities of 10^{4} - 10^{6} cm^{-3}, similiar to values obtained in larger beam studies which averaged over many shocks. There is also some evidence that shocks with higher densities have lower velocities., Comment: 33 pages, 11 figures, 2 of those color
Published: 2007
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18. Hubble Space Telescope NICMOS Polarization Measurements of OMC-1

Author: Simpson, Janet P., Colgan, Sean W. J., Erickson, Edwin F., Burton, Michael G., and Schultz, A. S. B.
Subjects: Astrophysics
Abstract: We present 2micron polarization measurements of positions in the BN region of the Orion Molecular Cloud (OMC-1) made with NICMOS Camera 2 (0.2'' resolution) on HST. Our results are as follows: BN is sim 29% polarized by dichroic absorption and appears to be the illuminating source for most of the nebulosity to its north and up to sim 5'' to its south. Although the stars are probably all polarized by dichroic absorption, there are a number of compact, but non-point-source, objects that could be polarized by a combination of both dichroic absorption and local scattering of star light. We identify several candidate YSOs, including an approximately edge-on bipolar YSO 8.7'' east of BN, and a deeply-embedded variable star. Additional strongly polarized sources are IRc2-B, IRc2-D, and IRc7, all of which are obviously self-luminous at mid-infrared wavelengths and may be YSOs. None of these is a reflection nebula illuminated by a star located near radio source I, as was previously suggested. Other IRc sources are clearly reflection nebulae: IRc3 appears to be illuminated by IRc2-B or a combination of the IRc2 sources, and IRc4 and IRc5 appear to be illuminated by an unseen star in the vicinity of radio source I, or by Star n or IRc2-A. Trends in the magnetic field direction are inferred from the polarization of the 26 stars that are bright enough to be seen as NICMOS point sources. The most polarized star has a polarization position angle different from its neighbors by sim 40^o, but in agreement with the grain alignment inferred from millimeter polarization measurements of the cold dust cloud in the southern part of OMC-1., Comment: 41 pages, 8 figures, 4 tables, to appear in The Astrophysical Journal
Published: 2006
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19. A CH3CN and HCO+ survey towards southern methanol masers associated with star formation

Author: Purcell, C. R., Balasubramanyam, R., Burton, M. G., Walsh, A. J., Minier, V., Hunt-Cunningham, M. R., Kedziora-Chudczer, L. L., Longmore, S. N., Hill, T., Bains, I., Barnes, P. J., Busfield, A. L., Calisse, P., Crighton, N. H. M., Curran, S. J., Davis, T. M., Dempsey, J. T., Derragopian, G., Fulton, B., Hidas, M. G., Hoare, M. G., Lee, J. -K., Ladd, E. F., Lumsden, S. L., Moore, T. J. T., Murphy, M. T., Oudmaijer, R. D., Pracy, M. B., Rathborne, J., Robertson, S., Schultz, A. S. B., Shobbrook, J., Sparks, P. A., Storey, J., and Travouillion, T.
Subjects: Astrophysics
Abstract: We present the initial results of a 3-mm spectral line survey towards 83 methanol maser selected massive star-forming regions. Here we report observations of the J=5-4 and 6-5 rotational transitions of methyl cyanide (CH3CN) and the J=1-0 transition of HCO+and H13CO+. CH3CN emission is detected in 58 sources (70 %) of our sample). We estimate the temperature and column density for 37 of these using the rotational diagram method. The temperatures we derive range from 28-166 K, and are lower than previously reported temperatures, derived from higher J transitions. We find that CH3CN is brighter and more commonly detected towards ultra-compact HII (UCHII) regions than towards isolated maser sources. Detection of CH3CN towards isolated maser sources strongly suggests that these objects are internally heated and that CH3CN is excited prior to the UCHII phase of massive star-formation. HCO+ is detected towards 82 sources (99 % of our sample), many of which exhibit asymmetric line profiles compared to H13CO+. Skewed profiles are indicative of inward or outward motions, however, we find approximately equal numbers of red and blue-skewed profiles among all classes. Column densities are derived from an analysis of the HCO+ and H13CO+ line profiles. 80 sources have mid-infrared counterparts: 68 seen in emission and 12 seen in absorption as `dark clouds'. Seven of the twelve dark clouds exhibit asymmetric HCO+ profiles, six of which are skewed to the blue, indicating infalling motions. CH3CN is also common in dark clouds, where it has a 90 % detection rate., Comment: 29 pages, 16 figures. Accepted for publication in MNRAS. For associated online figures please see http://www.phys.unsw.edu.au/~crp/papers/cpurcell_2005_online.pdf
Published: 2005
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20. HST NICMOS Observations of the Polarization of NGC 1068

Author: Simpson, Janet P., Colgan, Sean W. J., Erickson, Edwin F., Hines, Dean C., Schultz, A. S. B., and Trammell, Susan R.
Subjects: Astrophysics
Abstract: We have observed the polarized light at 2 micron in the center of NGC 1068 with HST NICMOS Camera 2. The nucleus is dominated by a bright, unresolved source, polarized at a level of 6.0 pm 1.2% with a position angle of 122degr pm 1.5degr. There are two polarized lobes extending up to 8'' northeast and southwest of the nucleus. The polarized flux in both lobes is quite clumpy, with the maximum polarization occurring in the southwest lobe at a level of 17% when smoothed to 0.23'' resolution. The perpendiculars to the polarization vectors in these two lobes point back to the intense unresolved nuclear source to within one 0.076'' Camera 2 pixel, thereby confirming that this is the illuminating source of the scattered light and therefore the probable AGN central engine. Whereas the polarization of the nucleus is probably caused by dichroic absorption, the polarization in the lobes is almost certainly caused by scattering, with very little contribution from dichroic absorption. Features in the polarized lobes include a gap at a distance of about 1'' from the nucleus toward the southwest lobe and a ``knot'' of emission about 5'' northeast of the nucleus. Both features had been discussed by ground-based observers, but they are much better defined with the high spatial resolution of NICMOS. The northeast knot may be the side of a molecular cloud that is facing the nucleus, which cloud may be preventing the expansion of the northeast radio lobe at the head of the radio synchrotron-radiation-emitting jet. We also report the presence of two ghosts in the Camera 2 polarizers. These had not been detected previously (Hines et al. 2000) because they are relatively faint and require observations of a source with a large dynamic range., Comment: 17 pages, 4 figures
Published: 2002
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21. The Optical Light Curve of GRB 221009A:The Afterglow and the Emerging Supernova

Author: Fulton, M. D., Smartt, S. J., Rhodes, L., Huber, M. E., Villar, V. A., Moore, T., Srivastav, S., Schultz, A. S. B., Chambers, K. C., Izzo, L., Hjorth, J., Chen, T.-w., Nicholl, M., Foley, R. J., Rest, A., Smith, K. W., Young, D. R., Sim, S. A., Bright, J., Zenati, Y., De Boer, T., Bulger, J., Fairlamb, J., Gao, H., Lin, C.-c., Lowe, T., Magnier, E. A., Smith, I. A., Wainscoat, R., Coulter, D. A., Jones, D. O., Kilpatrick, C. D., Mcgill, P., Ramirez-ruiz, E., Lee, K.-s., Narayan, G., Ramakrishnan, V., Ridden-harper, R., Singh, A., Wang, Q., Kong, A. K. H., Ngeow, C.-c., Pan, Y.-c., Yang, S., Davis, K. W., Piro, A. L., Rojas-bravo, C., Sommer, J., Yadavalli, S. K., Fulton, M. D., Smartt, S. J., Rhodes, L., Huber, M. E., Villar, V. A., Moore, T., Srivastav, S., Schultz, A. S. B., Chambers, K. C., Izzo, L., Hjorth, J., Chen, T.-w., Nicholl, M., Foley, R. J., Rest, A., Smith, K. W., Young, D. R., Sim, S. A., Bright, J., Zenati, Y., De Boer, T., Bulger, J., Fairlamb, J., Gao, H., Lin, C.-c., Lowe, T., Magnier, E. A., Smith, I. A., Wainscoat, R., Coulter, D. A., Jones, D. O., Kilpatrick, C. D., Mcgill, P., Ramirez-ruiz, E., Lee, K.-s., Narayan, G., Ramakrishnan, V., Ridden-harper, R., Singh, A., Wang, Q., Kong, A. K. H., Ngeow, C.-c., Pan, Y.-c., Yang, S., Davis, K. W., Piro, A. L., Rojas-bravo, C., Sommer, J., and Yadavalli, S. K.
Published: 2023

22. The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

Author: Fulton, M. D., primary, Smartt, S. J., additional, Rhodes, L., additional, Huber, M. E., additional, Villar, V. A., additional, Moore, T., additional, Srivastav, S., additional, Schultz, A. S. B., additional, Chambers, K. C., additional, Izzo, L., additional, Hjorth, J., additional, Chen, T.-W., additional, Nicholl, M., additional, Foley, R. J., additional, Rest, A., additional, Smith, K. W., additional, Young, D. R., additional, Sim, S. A., additional, Bright, J., additional, Zenati, Y., additional, de Boer, T., additional, Bulger, J., additional, Fairlamb, J., additional, Gao, H., additional, Lin, C.-C., additional, Lowe, T., additional, Magnier, E. A., additional, Smith, I. A., additional, Wainscoat, R., additional, Coulter, D. A., additional, Jones, D. O., additional, Kilpatrick, C. D., additional, McGill, P., additional, Ramirez-Ruiz, E., additional, Lee, K.-S., additional, Narayan, G., additional, Ramakrishnan, V., additional, Ridden-Harper, R., additional, Singh, A., additional, Wang, Q., additional, Kong, A. K. H., additional, Ngeow, C.-C., additional, Pan, Y.-C., additional, Yang, S., additional, Davis, K. W., additional, Piro, A. L., additional, Rojas-Bravo, C., additional, Sommer, J., additional, and Yadavalli, S. K., additional
Published: 2023
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23. PAHs as Probes of Photo-Dissociation Regions in M17 and the Orion Bar

Author: Sloan, G. C., Bregman, J., Schultz, A. S. B., Temi, P., Rank, D. M., Crane, Philippe, editor, Käufl, Hans Ulrich, editor, and Siebenmorgen, Ralf, editor
Published: 1996
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24. Shocked Molecular Hydrogen in the LkHα234 Region

Author: Schultz, A. S. B., Rank, D., Temi, P., Harker, D., Millar, T. J., editor, and Raga, A. C., editor
Published: 1995
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25. Observational constraints on the optical and near-infrared emission from the neutron star–black hole binary merger candidate S190814bv

Author: Ackley, K., primary, Amati, L., additional, Barbieri, C., additional, Bauer, F. E., additional, Benetti, S., additional, Bernardini, M. G., additional, Bhirombhakdi, K., additional, Botticella, M. T., additional, Branchesi, M., additional, Brocato, E., additional, Bruun, S. H., additional, Bulla, M., additional, Campana, S., additional, Cappellaro, E., additional, Castro-Tirado, A. J., additional, Chambers, K. C., additional, Chaty, S., additional, Chen, T.-W., additional, Ciolfi, R., additional, Coleiro, A., additional, Copperwheat, C. M., additional, Covino, S., additional, Cutter, R., additional, D’Ammando, F., additional, D’Avanzo, P., additional, De Cesare, G., additional, D’Elia, V., additional, Della Valle, M., additional, Denneau, L., additional, De Pasquale, M., additional, Dhillon, V. S., additional, Dyer, M. J., additional, Elias-Rosa, N., additional, Evans, P. A., additional, Eyles-Ferris, R. A. J., additional, Fiore, A., additional, Fraser, M., additional, Fruchter, A. S., additional, Fynbo, J. P. U., additional, Galbany, L., additional, Gall, C., additional, Galloway, D. K., additional, Getman, F. I., additional, Ghirlanda, G., additional, Gillanders, J. H., additional, Gomboc, A., additional, Gompertz, B. P., additional, González-Fernández, C., additional, González-Gaitán, S., additional, Grado, A., additional, Greco, G., additional, Gromadzki, M., additional, Groot, P. J., additional, Gutiérrez, C. P., additional, Heikkilä, T., additional, Heintz, K. E., additional, Hjorth, J., additional, Hu, Y.-D., additional, Huber, M. E., additional, Inserra, C., additional, Izzo, L., additional, Japelj, J., additional, Jerkstrand, A., additional, Jin, Z. P., additional, Jonker, P. G., additional, Kankare, E., additional, Kann, D. A., additional, Kennedy, M., additional, Kim, S., additional, Klose, S., additional, Kool, E. C., additional, Kotak, R., additional, Kuncarayakti, H., additional, Lamb, G. P., additional, Leloudas, G., additional, Levan, A. J., additional, Longo, F., additional, Lowe, T. B., additional, Lyman, J. D., additional, Magnier, E., additional, Maguire, K., additional, Maiorano, E., additional, Mandel, I., additional, Mapelli, M., additional, Mattila, S., additional, McBrien, O. R., additional, Melandri, A., additional, Michałowski, M. J., additional, Milvang-Jensen, B., additional, Moran, S., additional, Nicastro, L., additional, Nicholl, M., additional, Nicuesa Guelbenzu, A., additional, Nuttal, L., additional, Oates, S. R., additional, O’Brien, P. T., additional, Onori, F., additional, Palazzi, E., additional, Patricelli, B., additional, Perego, A., additional, Torres, M. A. P., additional, Perley, D. A., additional, Pian, E., additional, Pignata, G., additional, Piranomonte, S., additional, Poshyachinda, S., additional, Possenti, A., additional, Pumo, M. L., additional, Quirola-Vásquez, J., additional, Ragosta, F., additional, Ramsay, G., additional, Rau, A., additional, Rest, A., additional, Reynolds, T. M., additional, Rosetti, S. S., additional, Rossi, A., additional, Rosswog, S., additional, Sabha, N. B., additional, Sagués Carracedo, A., additional, Salafia, O. S., additional, Salmon, L., additional, Salvaterra, R., additional, Savaglio, S., additional, Sbordone, L., additional, Schady, P., additional, Schipani, P., additional, Schultz, A. S. B., additional, Schweyer, T., additional, Smartt, S. J., additional, Smith, K. W., additional, Smith, M., additional, Sollerman, J., additional, Srivastav, S., additional, Stanway, E. R., additional, Starling, R. L. C., additional, Steeghs, D., additional, Stratta, G., additional, Stubbs, C. W., additional, Tanvir, N. R., additional, Testa, V., additional, Thrane, E., additional, Tonry, J. L., additional, Turatto, M., additional, Ulaczyk, K., additional, van der Horst, A. J., additional, Vergani, S. D., additional, Walton, N. A., additional, Watson, D., additional, Wiersema, K., additional, Wiik, K., additional, Wyrzykowski, Ł., additional, Yang, S., additional, Yi, S.-X., additional, and Young, D. R., additional
Published: 2020
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26. Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger candidate S190814bv

Author: Ackley, K., Amati, L., Barbieri, C., Bauer, F. E., Benetti, S., Bernardini, M. G., Bhirombhakdi, K., Botticella, M. T., Branchesi, M., Brocato, E., Bruun, S. H., Bulla, Mattia, Campana, S., Cappellaro, E., Castro-Tirado, A. J., Chambers, K. C., Chaty, S., Chen, Ting-Wan, Ciolfi, R., Coleiro, A., Copperwheat, C. M., Covino, S., Cutter, R., D'Ammando, F., D'Avanzo, P., De Cesare, G., D'Elia, V., Della Valle, M., Denneau, L., De Pasquale, M., Dhillon, V. S., Dyer, M. J., Elias-Rosa, N., Evans, P. A., Eyles-Ferris, R. A. J., Fiore, A., Fraser, M., Fruchter, A. S., Fynbo, J. P. U., Galbany, L., Gall, C., Galloway, D. K., Getman, F., Ghirlanda, G., Gillanders, J. H., Gomboc, A., Gompertz, B. P., Gonzalez-Fernandez, C., Gonzalez-Gaitan, S., Grado, A., Greco, G., Gromadzki, M., Groot, P. J., Gutierrez, C. P., Heikkila, T., Heintz, K. E., Hjorth, J., Hu, Y.-D., Huber, M. E., Inserra, C., Izzo, L., Japelj, J., Jerkstrand, Anders, Jin, Z. P., Jonker, P. G., Kankare, E., Kann, D. A., Kennedy, M., Kim, S., Klose, S., Kool, Erik C., Kotak, R., Kuncarayakti, H., Lamb, G. P., Leloudas, G., Levan, A. J., Longo, F., Lowe, T. B., Lyman, J. D., Magnier, E., Maguire, K., Maiorano, E., Mandel, I., Mapelli, M., Mattila, S., McBrien, O. R., Melandri, A., Michalowski, M. J., Milvang-Jensen, B., Moran, S., Nicastro, L., Nicholl, M., Nicuesa Guelbenzu, A., Nuttal, L., Oates, S. R., O'Brien, P. T., Onori, F., Palazzi, E., Patricelli, B., Perego, A., Torres, M. A. P., Perley, D. A., Pian, E., Pignata, G., Piranomonte, S., Poshyachinda, S., Possenti, A., Pumo, M. L., Quirola-Vasquez, J., Ragosta, F., Ramsay, G., Rau, A., Rest, A., Reynolds, T. M., Rosetti, S. S., Rossi, A., Rosswog, Stephan, Sabha, N. B., Sagués Carracedo, Ana, Salafia, O. S., Salmon, L., Salvaterra, R., Savaglio, S., Sbordone, L., Schady, P., Schipani, P., Schultz, A. S. B., Schweyer, Tassilo, Smartt, S. J., Smith, K. W., Smith, M., Sollerman, Jesper, Srivastav, S., Stanway, E. R., Starling, R. L. C., Steeghs, D., Stratta, G., Stubbs, C. W., Tanvir, N. R., Testa, V., Thrane, E., Tonry, J. L., Turatto, M., Ulaczyk, K., van der Horst, A. J., Vergani, S. D., Walton, N. A., Watson, D., Wiersema, K., Wiik, K., Wyrzykowski, L., Yang, Sheng, Yi, S.-X., Young, D. R., Ackley, K., Amati, L., Barbieri, C., Bauer, F. E., Benetti, S., Bernardini, M. G., Bhirombhakdi, K., Botticella, M. T., Branchesi, M., Brocato, E., Bruun, S. H., Bulla, Mattia, Campana, S., Cappellaro, E., Castro-Tirado, A. J., Chambers, K. C., Chaty, S., Chen, Ting-Wan, Ciolfi, R., Coleiro, A., Copperwheat, C. M., Covino, S., Cutter, R., D'Ammando, F., D'Avanzo, P., De Cesare, G., D'Elia, V., Della Valle, M., Denneau, L., De Pasquale, M., Dhillon, V. S., Dyer, M. J., Elias-Rosa, N., Evans, P. A., Eyles-Ferris, R. A. J., Fiore, A., Fraser, M., Fruchter, A. S., Fynbo, J. P. U., Galbany, L., Gall, C., Galloway, D. K., Getman, F., Ghirlanda, G., Gillanders, J. H., Gomboc, A., Gompertz, B. P., Gonzalez-Fernandez, C., Gonzalez-Gaitan, S., Grado, A., Greco, G., Gromadzki, M., Groot, P. J., Gutierrez, C. P., Heikkila, T., Heintz, K. E., Hjorth, J., Hu, Y.-D., Huber, M. E., Inserra, C., Izzo, L., Japelj, J., Jerkstrand, Anders, Jin, Z. P., Jonker, P. G., Kankare, E., Kann, D. A., Kennedy, M., Kim, S., Klose, S., Kool, Erik C., Kotak, R., Kuncarayakti, H., Lamb, G. P., Leloudas, G., Levan, A. J., Longo, F., Lowe, T. B., Lyman, J. D., Magnier, E., Maguire, K., Maiorano, E., Mandel, I., Mapelli, M., Mattila, S., McBrien, O. R., Melandri, A., Michalowski, M. J., Milvang-Jensen, B., Moran, S., Nicastro, L., Nicholl, M., Nicuesa Guelbenzu, A., Nuttal, L., Oates, S. R., O'Brien, P. T., Onori, F., Palazzi, E., Patricelli, B., Perego, A., Torres, M. A. P., Perley, D. A., Pian, E., Pignata, G., Piranomonte, S., Poshyachinda, S., Possenti, A., Pumo, M. L., Quirola-Vasquez, J., Ragosta, F., Ramsay, G., Rau, A., Rest, A., Reynolds, T. M., Rosetti, S. S., Rossi, A., Rosswog, Stephan, Sabha, N. B., Sagués Carracedo, Ana, Salafia, O. S., Salmon, L., Salvaterra, R., Savaglio, S., Sbordone, L., Schady, P., Schipani, P., Schultz, A. S. B., Schweyer, Tassilo, Smartt, S. J., Smith, K. W., Smith, M., Sollerman, Jesper, Srivastav, S., Stanway, E. R., Starling, R. L. C., Steeghs, D., Stratta, G., Stubbs, C. W., Tanvir, N. R., Testa, V., Thrane, E., Tonry, J. L., Turatto, M., Ulaczyk, K., van der Horst, A. J., Vergani, S. D., Walton, N. A., Watson, D., Wiersema, K., Wiik, K., Wyrzykowski, L., Yang, Sheng, Yi, S.-X., and Young, D. R.
Abstract: Context. Gravitational wave (GW) astronomy has rapidly reached maturity, becoming a fundamental observing window for modern astrophysics. The coalescences of a few tens of black hole (BH) binaries have been detected, while the number of events possibly including a neutron star (NS) is still limited to a few. On 2019 August 14, the LIGO and Virgo interferometers detected a high-significance event labelled S190814bv. A preliminary analysis of the GW data suggests that the event was likely due to the merger of a compact binary system formed by a BH and a NS. Aims. In this paper, we present our extensive search campaign aimed at uncovering the potential optical and near infrared electromagnetic counterpart of S190814bv. We found no convincing electromagnetic counterpart in our data. We therefore use our non-detection to place limits on the properties of the putative outflows that could have been produced by the binary during and after the merger. Methods. Thanks to the three-detector observation of S190814bv, and given the characteristics of the signal, the LIGO and Virgo Collaborations delivered a relatively narrow localisation in low latency - a 50% (90%) credible area of 5 deg(2) (23 deg(2)) - despite the relatively large distance of 26752 Mpc. ElectromagNetic counterparts of GRAvitational wave sources at the VEry Large Telescope collaboration members carried out an intensive multi-epoch, multi-instrument observational campaign to identify the possible optical and near infrared counterpart of the event. In addition, the ATLAS, GOTO, GRAWITA-VST, Pan-STARRS, and VINROUGE projects also carried out a search on this event. In this paper, we describe the combined observational campaign of these groups. Results. Our observations allow us to place limits on the presence of any counterpart and discuss the implications for the kilonova (KN), which was possibly generated by this NS-BH merger, and for the strategy of future searches. The typical depth of our wide-field observat
Published: 2020
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27. YSE/Pan-STARRS1 Transient Discovery Report for 2020-01-31

Author: Jones, D. O., French, K. D., Agnello, A., Angus, C. R., Ansari, Z., Arendse, N., Gall, C., Grillo, C., Bruun, S. H., Hede, C., Hjorth, J., Izzo, L., Korhonen, H., Raimundo, S., Ramanah, D. K., Sarangi, A., Wojtak, R., Chambers, K. C., Huber, M. E., Magnier, E. A., Boer, T. J. L. D., Fairlamb, J. R., Lin, C. C., Wainscoat, R. J., Lowe, T., Willman, M., Bulger, J., Schultz, A. S. B., Engel, A., Gagliano, A., Narayan, G., Soraisam, M., Wang, Q., Rest, A., Smartt, S. J., Smith, K. W., Alexander, K., Baldeschi, A., Blanchard, P., Coppejans, D., DeMarchi, L., Hajela, A., Jacobson-Galan, W., Margutti, R., Matthews, D., Stauffer, C., Stroh, M., Terreran, G., Drout, M., Auchettl, K., Jones, D. O., French, K. D., Agnello, A., Angus, C. R., Ansari, Z., Arendse, N., Gall, C., Grillo, C., Bruun, S. H., Hede, C., Hjorth, J., Izzo, L., Korhonen, H., Raimundo, S., Ramanah, D. K., Sarangi, A., Wojtak, R., Chambers, K. C., Huber, M. E., Magnier, E. A., Boer, T. J. L. D., Fairlamb, J. R., Lin, C. C., Wainscoat, R. J., Lowe, T., Willman, M., Bulger, J., Schultz, A. S. B., Engel, A., Gagliano, A., Narayan, G., Soraisam, M., Wang, Q., Rest, A., Smartt, S. J., Smith, K. W., Alexander, K., Baldeschi, A., Blanchard, P., Coppejans, D., DeMarchi, L., Hajela, A., Jacobson-Galan, W., Margutti, R., Matthews, D., Stauffer, C., Stroh, M., Terreran, G., Drout, M., and Auchettl, K.
Abstract: Not Available
Published: 2020

28. Pan-STARRS1 Transient Discovery Report for 2020-01-08

Author: Jones, D. O., French, K. D., Agnello, A., Angus, C. R., Ansari, Z., Arendse, N., Gall, C., Grillo, C., Bruun, S. H., Hede, C., Hjorth, J., Izzo, L., Korhonen, H., Raimundo, S., Ramanah, D. K., Sarangi, A., Wojtak, R., Chambers, K. C., Huber, M. E., Magnier, E. A., Boer, T. J. L. D., Fairlamb, J. R., Lin, C. C., Wainscoat, R. J., Lowe, T., Willman, M., Bulger, J., Schultz, A. S. B., Engel, A., Gagliano, A., Narayan, G., Soraisam, M., Wang, Q., Rest, A., Smartt, S. J., Smith, K. W., Alexander, K., Baldeschi, A., Blanchard, P., Coppejans, D., DeMarchi, L., Hajela, A., Jacobson-Galan, W., Margutti, R., Matthews, D., Stauffer, C., Stroh, M., Terreran, G., Drout, M., Auchettl, K., Jones, D. O., French, K. D., Agnello, A., Angus, C. R., Ansari, Z., Arendse, N., Gall, C., Grillo, C., Bruun, S. H., Hede, C., Hjorth, J., Izzo, L., Korhonen, H., Raimundo, S., Ramanah, D. K., Sarangi, A., Wojtak, R., Chambers, K. C., Huber, M. E., Magnier, E. A., Boer, T. J. L. D., Fairlamb, J. R., Lin, C. C., Wainscoat, R. J., Lowe, T., Willman, M., Bulger, J., Schultz, A. S. B., Engel, A., Gagliano, A., Narayan, G., Soraisam, M., Wang, Q., Rest, A., Smartt, S. J., Smith, K. W., Alexander, K., Baldeschi, A., Blanchard, P., Coppejans, D., DeMarchi, L., Hajela, A., Jacobson-Galan, W., Margutti, R., Matthews, D., Stauffer, C., Stroh, M., Terreran, G., Drout, M., and Auchettl, K.
Published: 2020

29. Hubble Space Telescope NICMOS Polarization Measurements of OMC-1

Author: Simpson, Janet P, Colgan, Sean W. J, Erickson, Edwin F, Burton, Michael G, and Schultz, A. S. B
Subjects: Astronomy
Abstract: We present 2 micrometer polarization measurements of positions in the BN region of the Orion Molecular Cloud (OMC-1) made with NICMOS Camera 2 (0.2" resolution) on Hubble Space Telescope. Our goals are to seek the sources of heating for IRc2, 3, 4, and 7, identify possible young stellar objects (YSOs), and characterize the grain alignment in the dust clouds along the lines-of-sight to the stars. Our results are as follows: BN is approximately 29% polarized by dichroic absorption and appears to be the illuminating source for most of the nebulosity to its north and up to approximately 5" to its south. Although the stars are probably all polarized by dichroic absorption, there are a number of compact, but non-point-source, objects that could be polarized by a combination of both dichroic absorption and local scattering of star light. We identify several candidate YSOs, including an approximately edge-on bipolar YSO 8.7" east of BN, and a deeply-embedded IRc7, all of which are obviously self-luminous at mid-infrared wavelengths and may be YSOs. None of these is a reflection nebula illuminated by a star located near radio source I, as was previously suggested. Other IRc sources are clearly reflection nebulae: IRc3 appears to be illuminated by IRc2-B or a combination of the IRc2 sources, and IRc4 and IRc5 appear to be illuminated by an unseen star in the vicinity of radio source I, or by Star n or IRc2-A. Trends in the magnetic field direction are inferred from the polarization of the 26 stars that are bright enough to be seen as NICMOS point sources. Their polarization ranges from N less than or equal to 1% (all stars with this low polarization are optically visible) to greater than 40%. The most polarized star has a polarization position angle different from its neighbors by approximately 40 degrees, but in agreement with the grain alignment inferred from millimeter polarization measurements of the cold dust cloud in the southern part of OMC-1. The polarization position angle of another highly-polarized, probable star also requires a grain alignment and magnetic field orientation substantially different from the general magnetic field orientation of OMC-1.
Published: 2006

30. What's Going on Around BN

Author: Erickson, Edwin, Colgan, S. W. J, Schultz, A. S. B, Simpson, J. P, Burton, M. G, Kaufman, M. J, Young, E. T, and Stolovy, S
Subjects: Astronomy
Abstract: The Becklin-Neugebauer object, discovered in observations made by Eric Becklin as a graduate student, is the brightest mid-infrared source outside the solar system, and a beacon in the nearest region of massive star formation. Using NICMOS on HST, we have obtained near infrared photometric, spectroscopic, and polarimetric images of the region immediately around BN. These images, with resolutions < -0.2", reveal remarkable morphologies, shock details, new young stellar objects, faint stars with variable intensities, and outflow features. We will summarize these results and inferences regarding the shock properties, illuminating sources of the nebulosity, and IRc sources near BN.
Published: 2005

31. HST NICMOS Observations of the Polarization of NGC 1068

Author: Simpson, Janet P, Colgan, Sean W. J, Erickson, Edwin F, Hines, Dean C, Schultz, A. S. B, Trammell, Susan R, and DeVincenzi, D
Subjects: Astronomy
Abstract: We have observed the polarized light at 2 microns in the center of NGC 1068 with HST (Hubble Space Telescope) NICMOS (Near Infrared Camera Multi Object Spectrometer) Camera 2. The nucleus is dominated by a bright, unresolved source, polarized at a level of 6.0 +/- 1.2% with a position angle of 122 degrees +/- 1.5 degrees. There are two polarized lobes extending tip to 8" northeast and southwest of the nucleus. The polarized flux in both lobes is quite clumpy, with the maximum polarization occurring in the southwest lobe at a level of 17% when smoothed to 0.23" resolution. The perpendiculars to the polarization vectors in these two lobes point back to the intense unresolved nuclear source to within one 0.076" Camera 2 pixel, thereby confirming that this source is the origin of the scattered light and therefore the probable AGN (Active Galactic Nuclei) central engine. Whereas the polarization of the nucleus is probably caused by dichroic absorption, the polarization in the lobes is almost certainly caused by scattering, with very little contribution from dichroic absorption. Features in the polarized lobes include a gap at a distance of about 1" from the nucleus toward the southwest lobe and a "knot" of emission about 5" northwest of the nucleus. Both features had been discussed by groundbased observers, but they are much better defined with the high spatial resolution of NICMOS. The northeast knot may be the side of a molecular cloud that is facing the nucleus, which cloud may be preventing the expansion of the northeast radio lobe at the head of the radio synchrotron-radiation-emitting jet. We also report the presence of two ghosts in the Camera 2 polarizers.
Published: 2002

32. PAHs as Probes of Photo-Dissociation Regions in M17 and the Orion Bar

Author: Sloan, G. C., primary, Bregman, J., additional, Schultz, A. S. B., additional, Temi, P., additional, and Rank, D. M., additional
Published: 1996
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33. The Foundation Supernova Survey: Measuring Cosmological Parameters with Supernovae from a Single Telescope

Author: Jones, D. O., primary, Scolnic, D. M., additional, Foley, R. J., additional, Rest, A., additional, Kessler, R., additional, Challis, P. M., additional, Chambers, K. C., additional, Coulter, D. A., additional, Dettman, K. G., additional, Foley, M. M., additional, Huber, M. E., additional, Jha, S. W., additional, Johnson, E., additional, Kilpatrick, C. D., additional, Kirshner, R. P., additional, Manuel, J., additional, Narayan, G., additional, Pan, Y.-C., additional, Riess, A. G., additional, Schultz, A. S. B., additional, Siebert, M. R., additional, Berger, E., additional, Chornock, R., additional, Flewelling, H., additional, Magnier, E. A., additional, Smartt, S. J., additional, Smith, K. W., additional, Wainscoat, R. J., additional, Waters, C., additional, and Willman, M., additional
Published: 2019
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34. NICMOS Narrow-band Images of OMC-1

Author: Schultz, Angela S. B, Colgan, Sean W. J, Erickson, E. F, Kaufman, M. J, Hollenbach, D. J, O'Dell, C. R, Young, E. T, and Chen, H
Subjects: Astrophysics
Abstract: We present images of a 90in. x 90in. field centered on BN in OMC-1, taken with the Near-Infrared Camera and MultiObject Spectrograph (NICMOS) aboard the Hubble Space Telescope. The observed lines are H2 1-0 S(l), Pa, [FeII] 1.64 pm, and the adjacent continua. The region is rich in interesting structures. The most remarkable are the streamers or "fingers" of H2 emission which extend from 15in. to 50in. from IRc2, seen here in unprecedented detail. Unlike the northern H2 fingers, the inner fingers do not exhibit significant [FeII] emission at theirdips, which we suggest is due to lower excitation. These observations also show that the general morphology of the Pa and [FeII] emission (both imaged for the first time in this region) bears a striking resemblance to that of the Ha and [SII] emission previously observed with WFPC2. This implies that these IR and optical lines are produced by radiative excitation on the surface of the molecular cloud. The Pa morphology of HH 202 is also very similar to its H a and [OIII] emission, again suggesting that the Pa in this object is photo-excited by the Trapezium, as has been suggested for the optical emission. We find evidence of shock-excited [FeII] in HH 208, where it again closely follows the morphology of [SII]. There is also H2 coincident with the [SII] and [FeII] emission, which may be associated with HH 208. Finally, we note some interesting continuum features: diffuse "tails" trailing from IRc3 and IRc4, more extensive observations of the "crescent" found by Stolovy, et al. (1998), and new observations of a similar oval object nearby. We also find a "V"-shaped region which may be the boundary of a cavity being cleared by IRc2.
Published: 1998

35. Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the $Kepler$ 2 Observations

Author: Li, W., Wang, X., Vinkó, J., Mo, J., Hosseinzadeh, G., Sand, D. J., Zhang, J., Lin, H., Zhang, T., Wang, L., Chen, Z., Xiang, D., Rui, L., Huang, F., Li, X., Zhang, X., Li, L., Baron, E., Derkacy, J. M., Zhao, X., Sai, H., Zhang, K., Howell, D. A., McCully, C., Arcavi, I., Valenti, S., Hiramatsu, D., Burke, J., Rest, A., Garnavich, P., Tucker, B. E., Narayan, G., Shaya, E., Margheim, S., Zenteno, A., Villar, A., Dimitriadis, G., Foley, R. J., Pan, Y.-C., Coulter, D. A., Fox, O. D., Jha, S. W., Jones, D. O., Kasen, D. N., Kilpatrick, C. D., Piro, A. L., Riess, A. G., Rojas-Bravo, C., Shappee, B. J., Holoien, T. W.-S., Stanek, K. Z., Drout, M. R., Auchettl, K., Kochanek, C. S., Brown, J. S., Bose, S., Bersier, D., Brimacombe, J., Chen, P., Dong, S., Holmbo, S., Muñoz, J. A., Mutel, R. L., Post, R. S., Prieto, J. L., Shields, J., Tallon, D., Thompson, T. A., Vallely, P. J., Villanueva, S., Jr., Smartt, S. J., Smith, K. W., Chambers, K. C., Flewelling, H. A., Huber, M. E., Magnier, E. A., Waters, C. Z., Schultz, A. S. B., Bulger, J., Lowe, T. B., Willman, M., Sárneczky, K., Pál, A., Wheeler, J. C., Bódi, A., Bognár, Zs., Csák, B., Cseh, B., Csörnyei, G., Hanyecz, O., Ignácz, B., Kalup, Cs., Könyves-Tóth, R., Kriskovics, L., Ordasi, A., Rajmon, I., Sódor, A., Szabó, R., Szakáts, R., Zsidi, G., Milne, P., Andrews, J. E., Smith, N., Bilinski, C., Brown, P. J., Nordin, J., Williams, S. C., Galbany, L., Palmerio, J., Hook, I. M., Inserra, C., Maguire, K., Cartier, Régis, Razza, A., Gutiérrez, C. P., Hermes, J. J., Reding, J. S., Kaiser, B. C., Tonry, J. L., Heinze, A. N., Denneau, L., Weiland, H., Stalder, B., Barentsen, G., Dotson, J., Barclay, T., Gully-Santiago, M., Hedges, C., Cody, A. M., Howell, S., Coughlin, J., Van Cleve, J. E., Cardoso, J. Vinícius de Miranda, Larson, K. A., McCalmont-Everton, K. M., Peterson, C. A., Ross, S. E., Reedy, L. H., Osborne, D., McGinn, C., Kohnert, L., Migliorini, L., Wheaton, A., Spencer, B., Labonde, C., Castillo, G., Beerman, G., Steward, K., Hanley, M., Larsen, R., Gangopadhyay, R., Kloetzel, R., Weschler, T., Nystrom, V., Moffatt, J., Redick, M., Griest, K., Packard, M., Muszynski, M., Kampmeier, J., Bjella, R., Flynn, S., Elsaesser, B., Li, W., Wang, X., Vinkó, J., Mo, J., Hosseinzadeh, G., Sand, D. J., Zhang, J., Lin, H., Zhang, T., Wang, L., Chen, Z., Xiang, D., Rui, L., Huang, F., Li, X., Zhang, X., Li, L., Baron, E., Derkacy, J. M., Zhao, X., Sai, H., Zhang, K., Howell, D. A., McCully, C., Arcavi, I., Valenti, S., Hiramatsu, D., Burke, J., Rest, A., Garnavich, P., Tucker, B. E., Narayan, G., Shaya, E., Margheim, S., Zenteno, A., Villar, A., Dimitriadis, G., Foley, R. J., Pan, Y.-C., Coulter, D. A., Fox, O. D., Jha, S. W., Jones, D. O., Kasen, D. N., Kilpatrick, C. D., Piro, A. L., Riess, A. G., Rojas-Bravo, C., Shappee, B. J., Holoien, T. W.-S., Stanek, K. Z., Drout, M. R., Auchettl, K., Kochanek, C. S., Brown, J. S., Bose, S., Bersier, D., Brimacombe, J., Chen, P., Dong, S., Holmbo, S., Muñoz, J. A., Mutel, R. L., Post, R. S., Prieto, J. L., Shields, J., Tallon, D., Thompson, T. A., Vallely, P. J., Villanueva, S., Jr., Smartt, S. J., Smith, K. W., Chambers, K. C., Flewelling, H. A., Huber, M. E., Magnier, E. A., Waters, C. Z., Schultz, A. S. B., Bulger, J., Lowe, T. B., Willman, M., Sárneczky, K., Pál, A., Wheeler, J. C., Bódi, A., Bognár, Zs., Csák, B., Cseh, B., Csörnyei, G., Hanyecz, O., Ignácz, B., Kalup, Cs., Könyves-Tóth, R., Kriskovics, L., Ordasi, A., Rajmon, I., Sódor, A., Szabó, R., Szakáts, R., Zsidi, G., Milne, P., Andrews, J. E., Smith, N., Bilinski, C., Brown, P. J., Nordin, J., Williams, S. C., Galbany, L., Palmerio, J., Hook, I. M., Inserra, C., Maguire, K., Cartier, Régis, Razza, A., Gutiérrez, C. P., Hermes, J. J., Reding, J. S., Kaiser, B. C., Tonry, J. L., Heinze, A. N., Denneau, L., Weiland, H., Stalder, B., Barentsen, G., Dotson, J., Barclay, T., Gully-Santiago, M., Hedges, C., Cody, A. M., Howell, S., Coughlin, J., Van Cleve, J. E., Cardoso, J. Vinícius de Miranda, Larson, K. A., McCalmont-Everton, K. M., Peterson, C. A., Ross, S. E., Reedy, L. H., Osborne, D., McGinn, C., Kohnert, L., Migliorini, L., Wheaton, A., Spencer, B., Labonde, C., Castillo, G., Beerman, G., Steward, K., Hanley, M., Larsen, R., Gangopadhyay, R., Kloetzel, R., Weschler, T., Nystrom, V., Moffatt, J., Redick, M., Griest, K., Packard, M., Muszynski, M., Kampmeier, J., Bjella, R., Flynn, S., and Elsaesser, B.
Abstract: Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically-confirmed type Ia supernova (SN Ia) observed in the $Kepler$ field. The $Kepler$ data revealed an excess emission in its early light curve, allowing to place interesting constraints on its progenitor system (Dimitriadis et al. 2018, Shappee et al. 2018b). Here, we present extensive optical, ultraviolet, and near-infrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3$\pm$0.3 days and $\Delta$m$_{15}(B)=0.96\pm$0.03 mag, but it seems to have bluer $B - V$ colors. We construct the "uvoir" bolometric light curve having peak luminosity as 1.49$\times$10$^{43}$erg s$^{-1}$, from which we derive a nickel mass as 0.55$\pm$0.04M$_{\odot}$ by fitting radiation diffusion models powered by centrally located $^{56}$Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of $^{56}$Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a non-degenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia, but is characterized by prominent and persistent carbon absorption features. The C II features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in a SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.
Published: 2019

36. K2 Observations of SN 2018oh Reveal a Two-Component Rising Light Curve for a Type Ia Supernova

Author: Dimitriadis, G., Foley, R. J., Rest, A., Kasen, D., Piro, A. L., Polin, A., Jones, D. O., Villar, A., Narayan, G., Coulter, D. A., Kilpatrick, C. D., Pan, Y.-C., Rojas-Bravo, C., Fox, O. D., Jha, S. W., Nugent, P. E., Riess, A. G., Scolnic, D., Drout, M. R., Barentsen, G., Dotson, J., Gully-Santiago, M., Hedges, C., Cody, A. M., Barclay, T., Howell, S., Garnavich, P., Tucker, B. E., Shaya, E., Mushotzky, R., Olling, R. P., Margheim, S., Zenteno, A., Coughlin, J., Van Cleve, J. E., Cardoso, J. Vinicius de Miranda, Larson, K. A., McCalmont-Everton, K. M., Peterson, C. A., Ross, S. E., Reedy, L. H., Osborne, D., McGinn, C., Kohnert, L., Migliorini, L., Wheaton, A., Spencer, B., Labonde, C., Castillo, G., Beerman, G., Steward, K., Hanley, M., Larsen, R., Gangopadhyay, R., Kloetzel, R., Weschler, T., Nystrom, V., Moffatt, J., Redick, M., Griest, K., Packard, M., Muszynski, M., Kampmeier, J., Bjella, R., Flynn, S., Elsaesser, B., Chambers, K. C., Flewelling, H. A., Huber, M. E., Magnier, E. A., Waters, C. Z., Schultz, A. S. B., Bulger, J., Lowe, T. B., Willman, M., Smartt, S. J., Smith, K. W., Points, S., Strampelli, G. M., Brimacombe, J., Chen, P., Munoz, J. A., Mutel, R. L., Shields, J., Vallely, P. J., Villanueva, S., Jr, Li, W., Wang, X., Zhang, J., Lin, H., Mo, J., Zhao, X., Sai, H., Zhang, X., Zhang, K., Zhang, T., Wang, L., Baron, E., DerKacy, J. M., Li, L., Chen, Z., Xiang, D., Rui, L., Huang, F., Li, X., Hosseinzadeh, G., Howell, D. A., Arcavi, I., Hiramatsu, D., Burke, J., Valenti, S., Tonry, J. L., Denneau, L., Heinze, A. N., Weiland, H., Stalder, B., Vinko, J., Sarneczky, K., Pa, A., Bodi, A., Bognar, Zs., Csak, B., Cseh, B., Csornyei, G., Hanyecz, O., Ignacz, B., Kalup, Cs., Konyves-Toth, R., Kriskovics, L., Ordasi, A., Rajmon, I., Sodor, A., Szabo, R., Szakats, R., Zsidi, G., Williams, S. C., Nordin, J., Cartier, R., Frohmaier, C., Galbany, L., Gutierrez, C. P., Hook, I., Inserra, C., Smith, M., Sand, D. J., Andrews, J. E., Smith, N., Bilinski, C., Dimitriadis, G., Foley, R. J., Rest, A., Kasen, D., Piro, A. L., Polin, A., Jones, D. O., Villar, A., Narayan, G., Coulter, D. A., Kilpatrick, C. D., Pan, Y.-C., Rojas-Bravo, C., Fox, O. D., Jha, S. W., Nugent, P. E., Riess, A. G., Scolnic, D., Drout, M. R., Barentsen, G., Dotson, J., Gully-Santiago, M., Hedges, C., Cody, A. M., Barclay, T., Howell, S., Garnavich, P., Tucker, B. E., Shaya, E., Mushotzky, R., Olling, R. P., Margheim, S., Zenteno, A., Coughlin, J., Van Cleve, J. E., Cardoso, J. Vinicius de Miranda, Larson, K. A., McCalmont-Everton, K. M., Peterson, C. A., Ross, S. E., Reedy, L. H., Osborne, D., McGinn, C., Kohnert, L., Migliorini, L., Wheaton, A., Spencer, B., Labonde, C., Castillo, G., Beerman, G., Steward, K., Hanley, M., Larsen, R., Gangopadhyay, R., Kloetzel, R., Weschler, T., Nystrom, V., Moffatt, J., Redick, M., Griest, K., Packard, M., Muszynski, M., Kampmeier, J., Bjella, R., Flynn, S., Elsaesser, B., Chambers, K. C., Flewelling, H. A., Huber, M. E., Magnier, E. A., Waters, C. Z., Schultz, A. S. B., Bulger, J., Lowe, T. B., Willman, M., Smartt, S. J., Smith, K. W., Points, S., Strampelli, G. M., Brimacombe, J., Chen, P., Munoz, J. A., Mutel, R. L., Shields, J., Vallely, P. J., Villanueva, S., Jr, Li, W., Wang, X., Zhang, J., Lin, H., Mo, J., Zhao, X., Sai, H., Zhang, X., Zhang, K., Zhang, T., Wang, L., Baron, E., DerKacy, J. M., Li, L., Chen, Z., Xiang, D., Rui, L., Huang, F., Li, X., Hosseinzadeh, G., Howell, D. A., Arcavi, I., Hiramatsu, D., Burke, J., Valenti, S., Tonry, J. L., Denneau, L., Heinze, A. N., Weiland, H., Stalder, B., Vinko, J., Sarneczky, K., Pa, A., Bodi, A., Bognar, Zs., Csak, B., Cseh, B., Csornyei, G., Hanyecz, O., Ignacz, B., Kalup, Cs., Konyves-Toth, R., Kriskovics, L., Ordasi, A., Rajmon, I., Sodor, A., Szabo, R., Szakats, R., Zsidi, G., Williams, S. C., Nordin, J., Cartier, R., Frohmaier, C., Galbany, L., Gutierrez, C. P., Hook, I., Inserra, C., Smith, M., Sand, D. J., Andrews, J. E., Smith, N., and Bilinski, C.
Abstract: We present an exquisite, 30-min cadence Kepler (K2) light curve of the Type Ia supernova (SN Ia) 2018oh (ASASSN-18bt), starting weeks before explosion, covering the moment of explosion and the subsequent rise, and continuing past peak brightness. These data are supplemented by multi-color Pan-STARRS1 and CTIO 4-m DECam observations obtained within hours of explosion. The K2 light curve has an unusual two-component shape, where the flux rises with a steep linear gradient for the first few days, followed by a quadratic rise as seen for typical SNe Ia. This "flux excess" relative to canonical SN Ia behavior is confirmed in our $i$-band light curve, and furthermore, SN 2018oh is especially blue during the early epochs. The flux excess peaks 2.14$\pm0.04$ days after explosion, has a FWHM of 3.12$\pm0.04$ days, a blackbody temperature of $T=17,500^{+11,500}_{-9,000}$ K, a peak luminosity of $4.3\pm0.2\times10^{37}\,{\rm erg\,s^{-1}}$, and a total integrated energy of $1.27\pm0.01\times10^{43}\,{\rm erg}$. We compare SN 2018oh to several models that may provide additional heating at early times, including collision with a companion and a shallow concentration of radioactive nickel. While all of these models generally reproduce the early K2 light curve shape, we slightly favor a companion interaction, at a distance of $\sim$$2\times10^{12}\,{\rm cm}$ based on our early color measurements, although the exact distance depends on the uncertain viewing angle. Additional confirmation of a companion interaction in future modeling and observations of SN 2018oh would provide strong support for a single-degenerate progenitor system.
Published: 2019

37. Infrared, submillimeter, and millimeter observations of the soft gamma-ray repeaters

Author: Smith, I. A, Joyce, R, Schultz, A. S. B, Hurley, K, Vrba, F. J, Hartmann, D, Kouveliotou, C, vanParadijs, J, Waters, L. B. F. M, Chernin, L. M, Durouchoux, P, Corbel, S, and Wallyn, P
Subjects: Astronomy
Abstract: Soft gamma ray repeaters appear to be a new class of neutron stars. While a counterpart to SGR 0525-66 was detected uniquely in the X-ray band, SGR 1806-20 and SGR 1900+14 have unusual stellar counterparts whose spectra peak in the infrared. The infrared spectra appear to contain several components: the photospheric emission from stars dominates at shorter wavelengths; a bright point source dominates at 25 micrometers, and an extended source dominates at 60 micrometers. The longer wavelength spectra are inconsistent with mono-energetic synchrotron and black body radiation models. Recent millimeter, submillimeter and infrared observations are reviewed. A preliminary analysis of the higher resolution infrared spectra of SGR 1806-20 and SGR 1900+14 is outlined. These confirm previous observations suggesting that SGR1806-20 has an outflow and that the stars comprising the counterpart to SGR 1900+14 have very similar spectra.
Published: 1997

38. A Search for Structure in PAH Emission in Extended Sources at 3.3 and 3.4 Microns

Author: Bregman, Jesse, Temi, P, Rank, D. M, Sloan, G. C, Schultz, A. S. B, and Witteborn, Fred C
Subjects: Space Radiation
Abstract: We have observed three extended sources of the infrared emission features associated with polycyclic aromatic hydrocarbons (PAHs), using a 128x128 InSb array mounted on the 1.5 m NASA/Steward telescope on Mt. Lemmon. We used a CVF (1.5% bandpass) to isolate the emission from the 3.29 and 3.40 microns PAH features in NGC 1333 #3, Sharpless 106, and the Orion Bar. In all three sources, the 3.29 and 3.40 microns emission features arise from the same regions, but show decidedly different structure. We are analyzing the images to determine the relationship of the 3.40 microns feature to the main feature at 3.29 microns. The 3.40 microns feature may be a vibrational overtone of the 3.29 microns feature, or it may arise from attached molecular sidegroups.
Published: 1994

39. Searching for Super-fast Rotators Using the Pan-STARRS 1

Author: Chang, Chan-Kao, primary, Lin, Hsing-Wen, additional, Ip, Wing-Huen, additional, Chen, Wen-Ping, additional, Yeh, Ting-Shuo, additional, Chambers, K. C., additional, Magnier, E. A., additional, Huber, M. E., additional, Flewelling, H. A., additional, Waters, C. Z., additional, Wainscoat, R. J., additional, and Schultz, A. S. B., additional
Published: 2019
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40. Should Type Ia Supernova Distances Be Corrected for Their Local Environments?

Author: Jones, D. O., primary, Riess, A. G., additional, Scolnic, D. M., additional, Pan, Y.-C., additional, Johnson, E., additional, Coulter, D. A., additional, Dettman, K. G., additional, Foley, M. M., additional, Foley, R. J., additional, Huber, M. E., additional, Jha, S. W., additional, Kilpatrick, C. D., additional, Kirshner, R. P., additional, Rest, A., additional, Schultz, A. S. B., additional, and Siebert, M. R., additional
Published: 2018
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41. PanSTARRS1 Observations of the Kepler/K2 Campaign 16 and 17 Fields

Author: Dotson, Jessie L., primary, Rest, A., additional, Barentsen, Geert, additional, Gully-Santiago, Michael, additional, Fleming, Scott W., additional, Garnavich, P., additional, Tucker, B. E., additional, Kasen, D., additional, Narayan, G., additional, Shaya, E., additional, Olling, R., additional, Margheim, S., additional, Zenteno, A., additional, Villar, A., additional, Chambers, K. C., additional, Flewelling, H. A., additional, Huber, M. E., additional, Magnier, E. A., additional, Waters, C. Z., additional, Schultz, A. S. B., additional, Bulger, J., additional, Lowe, T. B., additional, Willman, M., additional, Smartt, S. J., additional, and Smith, K. W., additional
Published: 2018
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42. Multi-messenger Observations of a Binary Neutron Star Merger

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S. D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, Markus, Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calder, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, Ximeng, Chen, Y., Cheng, H. P., Chia, H., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, A. K. W., Chung, S., Ciani, G., Ciolfi, R., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. F., Cohen, D., Colla, A., Collette, C. G., Cominsky, L. R., Jr., M. Constancio, Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Dálya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C. F., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Day, B., De, S., DeBra, D., Degallaix, J., De Laurentis, M., Deléglise, S., Pozzo, W. Del, Demos, N., Denker, T., Dent, T., De Pietri, R., Dergachev, V., De Rosa, R., DeRosa, R. T., De Rossi, C., DeSalvo, R., De Varona, O., Devenson, J., Dhurandhar, S., Díaz, M. C., Fiore, L. Di, Giovanni, M. Di, Girolamo, T. Di, Lieto, A. Di, Pace, S. Di, Palma, I. Di, Renzo, F. Di, Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Douglas, R., Álvarez, M. Dovale, Downes, T. P., Drago, M., Dreissigacker, C., Driggers, J. C., Du, Z., Ducrot, M., Dupej, P., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenstein, R. A., Essick, R. C., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M. M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J. A., Forsyth, P. W. F., Forsyth, S. S., Fournier, J. D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E. M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Gretarsson, E. M., Griswold, B., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Haster, C. J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Houston, E. A., Howell, E. J., Hreibi, A., Hu, Y. M., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H. N., Isac, J. M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kasprzack, M., Katolik, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kéfélian, F., Keitel, D., Kemball, A. J., Kennedy, R., Kent, C., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. M., Kimbrell, S. J., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Krämer, C., Kringel, V., Krishnan, B., Królak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Landry, M., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Larson, S. L., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Li, T. G. F., Linker, S. D., Littenberg, T. B., Liu, J., Lo, R. K. L., Lockerbie, N. A., London, L. T., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D. M., Hernandez, I. Maga, Magaña-Sandoval, F., Zertuche, L. Maga, Magee, R. M., Majorana, E., Maksimovic, I., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsh, P., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McNeill, L., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Mejuto-Villa, E., Melatos, A., Mendell, G., Mercer, R. A., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, B. B., Miller, Julian Sebastian, Millhouse, M., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Ming, J., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moffa, D., Moggi, A., Mogushi, K., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mours, B., Mow-Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Napier, K., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Nevin, L., Newport, J. M., Newton, G., Ng, K. K. Y., Nguyen, P., Nguyen, Thank Thank, Nichols, D., Nielsen, A. B., Nissanke, S., Nitz, A., Noack, A., Nocera, F., Nolting, D., North, C., Nuttall, L. K., Oberling, J., O'Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard, O'Reilly, B., Ormiston, R., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Page, J., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perez, C. J., Perreca, A., Perri, L. M., Pfeiffer, H. P., Phelps, M., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pirello, M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Porter, E. K., Post, A., Powell, J., Prasad, J., Pratt, J. W. W., Pratten, G., Predoi, V., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Reyes, S. D., Ricci, F., Ricker, P. M., Rieger, S., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romel, C. L., Romie, J. H., Rosińska, D., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sampson, L. M., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Scheel, M., Scheuer, J., Schmidt, Jonathan, Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T. J., Shah, A. A., Shahriar, M. S., Shaner, M. B., Shao, L., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, A., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, B., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sonnenberg, J. A., Sorazu, B., Sorrentino, F., Souradeep, T., Spencer, A. P., Srivastava, A. K., Staats, K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sunil, S., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tápai, M., Taracchini, A., Tasson, J. D., Taylor, J. A., Taylor, R., Tewari, S. V., Theeg, T., Thies, F., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forné, A., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trinastic, J., Tringali, M. C., Trozzo, L., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Van Bakel, N., Van Beuzekom, Martinus, Van Den Brand, J. F. J., Van Den Broeck, C., Vander-Hyde, D. C., Van Der Schaaf, L., Van Heijningen, J. V., Van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Viceré, A., Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J. Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wessel, E. K., Wessels, P., Westerweck, J., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Whittle, C., Wilken, D., Williams, D., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J., Wong, K. W. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, S., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yu, Hang, Yu, Haocun, Yvert, M., Zadrożny, A., Zanolin, M., Zelenova, T., Zendri, J. P., Zevin, M., Zhang, L., Zhang, M., Zhang, T., Zhang, Y. H., Zhao, C., Zhou, M., Zhou, Z., Zhu, S. J., Zhu, X. J., Zimmerman, A. B., Zucker, M. E., Zweizig, J., Wilson-Hodge, C. A., Bissaldi, E., Blackburn, L., Briggs, M. S., Burns, E., Cleveland, W. H., Connaughton, V., Gibby, M. H., Giles, M. M., Goldstein, A., Hamburg, R., Jenke, P., Hui, C. M., Kippen, R. M., Kocevski, D., McBreen, S., Meegan, C. A., Paciesas, W. S., Poolakkil, S., Preece, R. D., Racusin, J., Roberts, O. J., Stanbro, M., Veres, P., Von Kienlin, A., Savchenko, V., Ferrigno, C., Kuulkers, E., Bazzano, A., Bozzo, E., Brandt, S., Chenevez, J., Courvoisier, T. J. L., Diehl, R., Domingo, A., Hanlon, L., Jourdain, E., Laurent, P., Lebrun, F., Lutovinov, A., Martin-Carrillo, A., Mereghetti, S., Rodi, J., Roques, J. P., Sunyaev, R., Ubertini, P., Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Samarai, I. Al, Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Argüelles, C., Auffenberg, Jan, Axani, S., Bagherpour, H., Bai, X., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. Becker, Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Börner, M., Bos, F., Bose, D., Böser, S., Botner, O., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Brayeur, L., Brenzke, M., Bretz, H. P., Bron, S., Brostean-Kaiser, J., Burgman, A., Carver, T., Casey, J., Casier, M., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Coenders, S., Collin, G. H., Conrad, J. M., Cowen, D. F., Cross, R., Day, M., De André, J. P. A. M., De Clercq, C., DeLaunay, J. J., Dembinski, H., De Ridder, S., Desiati, P., De Vries, K. D., De Wasseige, G., De With, M., DeYoung, T., Díaz-Vélez, J. C., Di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Flis, S., Franckowiak, A., Friedman, E., Fuchs, T., Gaisser, T. K., Gallagher, J., Gerhardt, L., Ghorbani, K., Giang, W., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, Christian, Hallgren, A., Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., Hünnefeld, M., In, S., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kalaczynski, P., Kang, W., Kappes, A., Karg, T., Karle, A., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kim, M., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Kohnen, G., Koirala, R., Kolanoski, H., Köpke, L., Kopper, C., Kopper, S., Koschinsky, J. P., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Krückl, G., Kunnen, J., Kunwar, S., Kurahashi, N., Kuwabara, T., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Lesiak-Bzdak, M., Leuermann, Martin, Liu, Q. R., Lu, L., Lünemann, J., Luszczak, W., Madsen, J., Maggi, G., Mahn, K. B. 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Abstract: 59 Seiten : Illustrationen, Tabellen, Diagramme (2017).
Published: 2017
Full Text: View/download PDF

43. Multi-messenger Observations of a Binary Neutron Star Merger

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S. D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H.-P., Chia, H., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, A. K. W., Chung, S., Ciani, G., Ciolfi, R., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P.-F., Cohen, D., Colla, A., Collette, C. G., Cominsky, L. R., Jr., M. Constancio, Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J.-P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dálya, G., Danilishin, S. L., D’Antonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C. F., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Day, B., De, S., DeBra, D., Degallaix, J., Laurentis, M. De, Deléglise, S., Pozzo, W. Del, Demos, N., Denker, T., Dent, T., Pietri, R. De, Dergachev, V., Rosa, R. De, DeRosa, R. T., Rossi, C. De, DeSalvo, R., Varona, O. de, Devenson, J., Dhurandhar, S., Díaz, M. C., Fiore, L. Di, Giovanni, M. Di, Girolamo, T. Di, Lieto, A. Di, Pace, S. Di, Palma, I. Di, Renzo, F. Di, Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Douglas, R., Álvarez, M. Dovale, Downes, T. P., Drago, M., Dreissigacker, C., Driggers, J. C., Du, Z., Ducrot, M., Dupej, P., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenstein, R. A., Essick, R. C., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M. M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J. A., Forsyth, P. W. F., Forsyth, S. S., Fournier, J.-D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E. M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Gretarsson, E. M., Griswold, B., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Haster, C.-J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Houston, E. A., Howell, E. J., Hreibi, A., Hu, Y. M., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H. N., Isac, J.-M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kasprzack, M., Katolik, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kéfélian, F., Keitel, D., Kemball, A. J., Kennedy, R., Kent, C., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y.-M., Kimbrell, S. J., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Krämer, C., Kringel, V., Krishnan, B., Królak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Landry, M., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Larson, S. L., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Li, T. G. F., Linker, S. D., Littenberg, T. B., Liu, J., Lo, R. K. L., Lockerbie, N. A., London, L. T., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D. M., Hernandez, I. Magaña, Magaña-Sandoval, F., Zertuche, L. Magaña, Magee, R. M., Majorana, E., Maksimovic, I., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsh, P., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McNeill, L., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Mejuto-Villa, E., Melatos, A., Mendell, G., Mercer, R. A., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, B. B., Miller, J., Millhouse, M., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Ming, J., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moffa, D., Moggi, A., Mogushi, K., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mours, B., Mow-Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Napier, K., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Nevin, L., Newport, J. M., Newton, G., Ng, K. K. Y., Nguyen, P., Nguyen, T. T., Nichols, D., Nielsen, A. B., Nissanke, S., Nitz, A., Noack, A., Nocera, F., Nolting, D., North, C., Nuttall, L. K., Oberling, J., O’Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O’Reilly, B., Ormiston, R., Ortega, L. F., O’Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Page, J., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perez, C. J., Perreca, A., Perri, L. M., Pfeiffer, H. P., Phelps, M., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pirello, M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Porter, E. K., Post, A., Powell, J., Prasad, J., Pratt, J. W. W., Pratten, G., Predoi, V., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Reyes, S. D., Ricci, F., Ricker, P. M., Rieger, S., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romel, C. L., Romie, J. H., Rosińska, D., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sampson, L. M., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Scheel, M., Scheuer, J., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T. J., Shah, A. A., Shahriar, M. S., Shaner, M. B., Shao, L., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, A., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, B., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sonnenberg, J. A., Sorazu, B., Sorrentino, F., Souradeep, T., Spencer, A. P., Srivastava, A. K., Staats, K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sunil, S., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tápai, M., Taracchini, A., Tasson, J. D., Taylor, J. A., Taylor, R., Tewari, S. V., Theeg, T., Thies, F., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forné, A., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trinastic, J., Tringali, M. C., Trozzo, L., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Bakel, N. van, Beuzekom, M. van, van den Brand, J. F. J., Van Den Broeck, C., Vander-Hyde, D. C., van der Schaaf, L., Heijningen, J. V. van, Veggel, A. A. van, Vardaro, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Viceré, A., Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J.-Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L.-W., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wessel, E. K., Wessels, P., Westerweck, J., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Whittle, C., Wilken, D., Williams, D., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J., Wong, K. W. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, S., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yu, Hang, Yu, Haocun, Yvert, M., Zadrożny, A., Zanolin, M., Zelenova, T., Zendri, J.-P., Zevin, M., Zhang, L., Zhang, M., Zhang, T., Zhang, Y.-H., Zhao, C., Zhou, M., Zhou, Z., Zhu, S. J., Zhu, X. J., Zimmerman, A. B., Zucker, M. E., Zweizig, J., Wilson-Hodge, C. A., Bissaldi, E., Blackburn, L., Briggs, M. S., Burns, E., Cleveland, W. H., Connaughton, V., Gibby, M. H., Giles, M. M, Goldstein, A., Hamburg, R., Jenke, P., Hui, C. M., Kippen, R. M., Kocevski, D., McBreen, S., Meegan, C. A., Paciesas, W. S., Poolakkil, S., Preece, R. D., Racusin, J., Roberts, O. J., Stanbro, M., Veres, P., von Kienlin, A., Savchenko, V., Ferrigno, C., Kuulkers, E., Bazzano, A., Bozzo, E., Brandt, S., Chenevez, J., Courvoisier, T. J.-L., Diehl, R., Domingo, A., Hanlon, L., Jourdain, E., Laurent, P., Lebrun, F., Lutovinov, A., Martin-Carrillo, A., Mereghetti, S., Natalucci, L., Rodi, J., Roques, J.-P., Sunyaev, R., Ubertini, P., Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Samarai, I. Al, Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Argüelles, C., Auffenberg, J., Axani, S., Bagherpour, H., Bai, X., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. Becker, Bernardini, E., Besson, D. 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M., Paxman, J., Sansom, E. K., Towner, M. C., Tonry, J., Coughlin, M., Stubbs, C. W., Denneau, L., Heinze, A., Stalder, B., Weiland, H., Eatough, R. P., Kramer, M., Kraus, A., Piro, L., González, J. Becerra, Butler, N. R., Khandrika, H. G., Kutyrev, A., Lee, W. H., Ricci, R., Ryan Jr., R. E., Sánchez-Ramírez, R., Veilleux, S., Watson, A. M., Wieringa, M. H., Burgess, J. M., Eerten, H. van, Fontes, C. J., Korobkin, O., Wollaeger, R. T., Camilo, F., Foley, A. R., Goedhart, S., Makhathini, S., Oozeer, N., Smirnov, O. M., and Woudt, P. A.
Subjects: ddc
Published: 2016

44. The Foundation Supernova Survey: motivation, design, implementation, and first data release

Author: Foley, Ryan J, primary, Scolnic, Daniel, additional, Rest, Armin, additional, Jha, S W, additional, Pan, Y-C, additional, Riess, A G, additional, Challis, P, additional, Chambers, K C, additional, Coulter, D A, additional, Dettman, K G, additional, Foley, M M, additional, Fox, O D, additional, Huber, M E, additional, Jones, D O, additional, Kilpatrick, C D, additional, Kirshner, R P, additional, Schultz, A S B, additional, Siebert, M R, additional, Flewelling, H A, additional, Gibson, B, additional, Magnier, E A, additional, Miller, J A, additional, Primak, N, additional, Smartt, S J, additional, Smith, K W, additional, Wainscoat, R J, additional, Waters, C, additional, and Willman, M, additional
Published: 2017
Full Text: View/download PDF

45. Observations of the GRB Afterglow ATLAS17aeu and Its Possible Association with GW 170104

Author: Stalder, B., primary, Tonry, J., additional, Smartt, S. J., additional, Coughlin, M., additional, Chambers, K. C., additional, Stubbs, C. W., additional, Chen, T.-W., additional, Kankare, E., additional, Smith, K. W., additional, Denneau, L., additional, Sherstyuk, A., additional, Heinze, A., additional, Weiland, H., additional, Rest, A., additional, Young, D. R., additional, Huber, M. E., additional, Flewelling, H., additional, Lowe, T., additional, Magnier, E. A., additional, Schultz, A. S. B., additional, Waters, C., additional, Wainscoat, R., additional, Willman, M., additional, Wright, D. E., additional, Chu, J., additional, Sanders, D., additional, Inserra, C., additional, Maguire, K., additional, and Kotak, R., additional
Published: 2017
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46. A kilonova as the electromagnetic counterpart to a gravitational-wave source

Author: Smartt, S. J., primary, Chen, T.-W., additional, Jerkstrand, A., additional, Coughlin, M., additional, Kankare, E., additional, Sim, S. A., additional, Fraser, M., additional, Inserra, C., additional, Maguire, K., additional, Chambers, K. C., additional, Huber, M. E., additional, Krühler, T., additional, Leloudas, G., additional, Magee, M., additional, Shingles, L. J., additional, Smith, K. W., additional, Young, D. R., additional, Tonry, J., additional, Kotak, R., additional, Gal-Yam, A., additional, Lyman, J. D., additional, Homan, D. S., additional, Agliozzo, C., additional, Anderson, J. P., additional, Angus, C. R., additional, Ashall, C., additional, Barbarino, C., additional, Bauer, F. E., additional, Berton, M., additional, Botticella, M. T., additional, Bulla, M., additional, Bulger, J., additional, Cannizzaro, G., additional, Cano, Z., additional, Cartier, R., additional, Cikota, A., additional, Clark, P., additional, De Cia, A., additional, Della Valle, M., additional, Denneau, L., additional, Dennefeld, M., additional, Dessart, L., additional, Dimitriadis, G., additional, Elias-Rosa, N., additional, Firth, R. E., additional, Flewelling, H., additional, Flörs, A., additional, Franckowiak, A., additional, Frohmaier, C., additional, Galbany, L., additional, González-Gaitán, S., additional, Greiner, J., additional, Gromadzki, M., additional, Guelbenzu, A. Nicuesa, additional, Gutiérrez, C. P., additional, Hamanowicz, A., additional, Hanlon, L., additional, Harmanen, J., additional, Heintz, K. E., additional, Heinze, A., additional, Hernandez, M.-S., additional, Hodgkin, S. T., additional, Hook, I. M., additional, Izzo, L., additional, James, P. A., additional, Jonker, P. G., additional, Kerzendorf, W. E., additional, Klose, S., additional, Kostrzewa-Rutkowska, Z., additional, Kowalski, M., additional, Kromer, M., additional, Kuncarayakti, H., additional, Lawrence, A., additional, Lowe, T. B., additional, Magnier, E. A., additional, Manulis, I., additional, Martin-Carrillo, A., additional, Mattila, S., additional, McBrien, O., additional, Müller, A., additional, Nordin, J., additional, O’Neill, D., additional, Onori, F., additional, Palmerio, J. T., additional, Pastorello, A., additional, Patat, F., additional, Pignata, G., additional, Podsiadlowski, Ph., additional, Pumo, M. L., additional, Prentice, S. J., additional, Rau, A., additional, Razza, A., additional, Rest, A., additional, Reynolds, T., additional, Roy, R., additional, Ruiter, A. J., additional, Rybicki, K. A., additional, Salmon, L., additional, Schady, P., additional, Schultz, A. S. B., additional, Schweyer, T., additional, Seitenzahl, I. R., additional, Smith, M., additional, Sollerman, J., additional, Stalder, B., additional, Stubbs, C. W., additional, Sullivan, M., additional, Szegedi, H., additional, Taddia, F., additional, Taubenberger, S., additional, Terreran, G., additional, van Soelen, B., additional, Vos, J., additional, Wainscoat, R. J., additional, Walton, N. A., additional, Waters, C., additional, Weiland, H., additional, Willman, M., additional, Wiseman, P., additional, Wright, D. E., additional, Wyrzykowski, Ł., additional, and Yaron, O., additional
Published: 2017
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47. A SEARCH FOR AN OPTICAL COUNTERPART TO THE GRAVITATIONAL-WAVE EVENT GW151226

Author: Smartt, S. J., primary, Chambers, K. C., additional, Smith, K. W., additional, Huber, M. E., additional, Young, D. R., additional, Chen, T.-W., additional, Inserra, C., additional, Wright, D. E., additional, Coughlin, M., additional, Denneau, L., additional, Flewelling, H., additional, Heinze, A., additional, Jerkstrand, A., additional, Magnier, E. A., additional, Maguire, K., additional, Mueller, B., additional, Rest, A., additional, Sherstyuk, A., additional, Stalder, B., additional, Schultz, A. S. B., additional, Stubbs, C. W., additional, Tonry, J., additional, Waters, C., additional, Wainscoat, R. J., additional, Valle, M. Della, additional, Dennefeld, M., additional, Dimitriadis, G., additional, Firth, R. E., additional, Fraser, M., additional, Frohmaier, C., additional, Gal-Yam, A., additional, Harmanen, J., additional, Kankare, E., additional, Kotak, R., additional, Kromer, M., additional, Mandel, I., additional, Sollerman, J., additional, Gibson, B., additional, Primak, N., additional, and Willman, M., additional
Published: 2016
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48. Pan-STARRS and PESSTO search for an optical counterpart to the LIGO gravitational-wave source GW150914

Author: Smartt, S. J., primary, Chambers, K. C., additional, Smith, K. W., additional, Huber, M. E., additional, Young, D. R., additional, Cappellaro, E., additional, Wright, D. E., additional, Coughlin, M., additional, Schultz, A. S. B., additional, Denneau, L., additional, Flewelling, H., additional, Heinze, A., additional, Magnier, E. A., additional, Primak, N., additional, Rest, A., additional, Sherstyuk, A., additional, Stalder, B., additional, Stubbs, C. W., additional, Tonry, J., additional, Waters, C., additional, Willman, M., additional, Anderson, J. P., additional, Baltay, C., additional, Botticella, M. T., additional, Campbell, H., additional, Dennefeld, M., additional, Chen, T.-W., additional, Della Valle, M., additional, Elias-Rosa, N., additional, Fraser, M., additional, Inserra, C., additional, Kankare, E., additional, Kotak, R., additional, Kupfer, T., additional, Harmanen, J., additional, Galbany, L., additional, Gal-Yam, A., additional, Le Guillou, L., additional, Lyman, J. D., additional, Maguire, K., additional, Mitra, A., additional, Nicholl, M., additional, Olivares E, F., additional, Rabinowitz, D., additional, Razza, A., additional, Sollerman, J., additional, Smith, M., additional, Terreran, G., additional, Valenti, S., additional, Gibson, B., additional, and Goggia, T., additional
Published: 2016
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49. The Foundation Supernova Survey: motivation, design, implementation, and first data release.

Author: Foley, Ryan J., Scolnic, Daniel, Rest, Armin, Jha, S. W., Pan, Y.-C., Riess, A. G., Challis, P., Chambers, K. C., Coulter, D. A., Dettman, K. G., Foley, M. M., Fox, O. D., Huber, M. E., Jones, D. O., Kilpatrick, C. D., Kirshner, R. P., Schultz, A. S. B., Siebert, M. R., Flewelling, H. A., and Gibson, B.
Subjects: TYPE I supernovae, ASTRONOMICAL observations, TELESCOPES, GALACTIC redshift, DARK energy
Abstract: The Foundation Supernova Survey aims to provide a large, high-fidelity, homogeneous, and precisely calibrated low-redshift Type Ia supernova (SN Ia) sample for cosmology. The calibration of the current low-redshift SN sample is the largest component of systematic uncertainties for SN cosmology, and new data are necessary to make progress. We present the motivation, survey design, observation strategy, implementation, and first results for the Foundation Supernova Survey. We are using the Pan-STARRS telescope to obtain photometry for up to 800 SNe Ia at z≲0.1. This strategy has several unique advantages: (1) the Pan-STARRS system is a superbly calibrated telescopic system, (2) Pan-STARRS has observed 3/4 of the sky in grizyP1 making future template observations unnecessary, (3) we have a well-tested data-reduction pipeline, and (4) we have observed ∼3000 high-redshift SNe Ia on this system. Here, we present our initial sample of 225 SN Ia grizP1 light curves, of which 180 pass all criteria for inclusion in a cosmological sample. The Foundation Supernova Survey already contains more cosmologically useful SNe Ia than all other published low-redshift SN Ia samples combined. We expect that the systematic uncertainties for the Foundation Supernova Sample will be two to three times smaller than other low-redshift samples.We find that our cosmologically useful sample has an intrinsic scatter of 0.111 mag, smaller than other low-redshift samples. We perform detailed simulations showing that simply replacing the current low-redshift SN Ia sample with an equally sized Foundation sample will improve the precision on the dark energy equation-of-state parameter by 35 per cent, and the dark energy figure of merit by 72 per cent. [ABSTRACT FROM AUTHOR]
Published: 2018
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50. Infrared observations of soft gamma repeaters

Author: Paradijs, J., Waters, L. B. F. M., Paul Groot, Kouveliotou, C., Smith, I. A., Hurley, K. C., Schultz, A. S. B., Wallyn, P., Telesco, C., Hooft, F., Bontekoe, T. R., Kester, D. J. M., and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Published: 1996

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