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Your search keyword '"Franzen, T. M. O."' showing total 35 results
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35 results on '"Franzen, T. M. O."'

1. Characterization of the AARTFAAC-12 aperture array: radio source counts at 42 and 61 MHz.

Author

Shulevski, A, Franzen, T M O, Williams, W L, Vernstrom, T, Gehlot, B K, Kuiack, M, and Wijers, R A M J

Subjects
*SIGNAL processing, *ACQUISITION of data, *TELESCOPES
Abstract

Dense aperture arrays provide key benefits in modern astrophysical research. They are flexible, employing cheap receivers, while relying on the ever more sophisticated compute back end to deal with the complexities of signal processing required for optimal use. Their advantage is that they offer very large fields of view and are readily scalable to any size, all other things being equal. Since they represent 'software telescopes', the science cases these arrays can be applied to are quite broad. Here, we describe the calibration and performance of the AARTFAAC-12 instrument, which is composed of the twelve centrally located stations of the LOFAR array. We go into the details of the data acquisition and pre-processing, we describe the newly developed calibration pipeline as well as the noise properties of the resulting images and present radio source counts at 41.7 MHz and 61 MHz. We find that AARTFAAC-12 is confusion limited at 0.9 Jy/PSF at 61 MHz with a PSF size of 17 × 11 arcmin and that the normalized source counts agree with the scaled VLSSr and 6C survey counts. The median spectral index of the sources between the two frequencies we observed at is -0.78. Further, we have used the derived source counts to estimate any excess cosmic radio background, and we do not find evidence for it at our observing frequencies compared to published literature values. [ABSTRACT FROM AUTHOR]

Published
2022
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2. First Season MWA Phase II EoR Power Spectrum Results at Redshift 7

Author

Li, W., Pober, J. C., Barry, N., Hazelton, B. J., Morales, M. F., Trott, C. M., Lanman, A., Wilensky, M., Sullivan, I., Beardsley, A. P., Booler, T., Bowman, J. D., Byrne, R., Crosse, B., Emrich, D., Franzen, T. M. O., Hasegawa, K., Horsley, L., Johnston-Hollitt, M., Jacobs, D. C., Jordan, C. H., Joseph, R. C., Kaneuji, T., Kaplan, D. L., Kenney, D., Kubota, K., Line, J., Lynch, C., McKinley, B., Mitchell, D. A., Murray, S., Pallot, D., Pindor, B., Rahimi, M., Riding, J., Sleap, G., Steele, K., Takahashi, K., Tingay, S. J., Walker, M., Wayth, R. B., Webster, R. L., Williams, A., Wu, C., Wyithe, J. S. B., Yoshiura, S., and Zheng, Q.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The compact configuration of Phase II of the Murchison Widefield Array (MWA) consists of both a redundant subarray and pseudo-random baselines, offering unique opportunities to perform sky-model and redundant interferometric calibration. The highly redundant hexagonal cores give improved power spectrum sensitivity. In this paper, we present the analysis of nearly 40 hours of data targeting one of the MWA's EoR fields observed in 2016. We use both improved analysis techniques presented in Barry et al. (2019) as well as several additional techniques developed for this work, including data quality control methods and interferometric calibration approaches. We show the EoR power spectrum limits at redshift 6.5, 6.8 and 7.1 based on our deep analysis on this 40-hour data set. These limits span a range in $k$ space of $0.18$ $h$ $\mathrm{Mpc^{-1}}$ $, Comment: 26 pages, 15 figures, 3 tables. Updated acknowledgements. Published in ApJ

Published
2019

3. New candidate radio supernova remnants detected in the GLEAM survey over 345° < l < 60°, 180° < l < 240°

Author

Hurley-Walker, N., Filipović, M. D., Gaensler, B. M., Leahy, D. A., Hancock, P. J., Franzen, T. M. O., Offringa, A. R., Callingham, J. R., Hindson, L., Wu, C., Bell, M. E., For, B. -Q., Johnston-Hollitt, M., Kapińska, A. D., Morgan, J., Murphy, T., McKinley, B., Procopio, P., Staveley-Smith, L., Wayth, R. B., Zheng, Q., and Astronomy

Subjects
G 356.5 - 1.9, G 358.3 - 0.7, G 18.9 - 1.2, G 350.8 + 5.0, G 355.4 + 2.7, G 349.1 - 0.8, G 21.8 + 0.2, G 7.4 + 0.3, G 19.7 - 0.7, G 23.1 + 0.1, supernovae: general, G 351.0 - 0.6, G 24.0 - 0.3, G 25.3 - 1.8, G 351.4 + 0.2, ISM: individual objects: G 0.1, G 351.4 + 0.4, G 230.4 + 1.2, G 351.9 + 0.1, ISM: supernova remnants, G 20.1 - 0.2, G 2.1 + 2.7, Astrophysics - Astrophysics of Galaxies, G 350.7 + 0.6, G 353.0 + 0.8, G 232.1 + 2.0, radio continuum: ISM, G 19.1 - 3.1, G 28.3 + 0.2, G 35.3 - 0.0, G 28.7 - 0.4, Astrophysics - High Energy Astrophysical Phenomena, 9.7
Abstract

We have detected 27 new supernova remnants (SNRs) using a new data release of the GLEAM survey from the Murchison Widefield Array telescope, including the lowest surface brightness SNR ever detected, G 0.1 - 9.7. Our method uses spectral fitting to the radio continuum to derive spectral indices for 26/27 candidates, and our low-frequency observations probe a steeper spectrum population than previously discovered. None of the candidates have coincident WISE mid-IR emission, further showing that the emission is non-thermal. Using pulsar associations we derive physical properties for six candidate SNRs, finding G 0.1 - 9.7 may be younger than 10 kyr. Sixty per cent of the candidates subtend areas larger than 0.2 deg2 on the sky, compared to < 25% of previously detected SNRs. We also make the first detection of two SNRs in the Galactic longitude range 220°-240°.

Published
2019

4. Candidate radio supernova remnants observed by the GLEAM survey over 345° < l < 60° and 180° < l < 240°

Author

Hurley-Walker, N., Gaensler, B. M., Leahy, D. A., Filipović, M. D., Hancock, P. J., Franzen, T. M. O., Offringa, A. R., Callingham, J. R., Hindson, L., Wu, C., Bell, M. E., For, B. -Q., Johnston-Hollitt, M., Kapińska, A. D., Morgan, J., Murphy, T., McKinley, B., Procopio, P., Staveley-Smith, L., Wayth, R. B., Zheng, Q., and Astronomy

Subjects
G359.2-01.1, G13.1-0.5, G353.3-1.1, G09. 6833-0.0667, G18.7583-0.0736, ISM: individual objects: G189.6 + 3.3, G36.00+0.00, supernovae: general, G7.5-1.7, G20.4667+0.1500, G356.6+00.1, G28.3750+0.2028, ISM: supernova remnants, G354.46+0.07, G345.1-0.2, G345.1+0.2, radiation mechanisms: non-thermal, G15.51-0.15, G19.00-0.35, Astrophysics - Astrophysics of Galaxies, G18.6375-0.2917, G348.8+1.1, radio continuum: ISM, G1.2-0.0, G005.3+0.1, G27.1333+0.0333, G28.7667-0.4250, G352.2-0.1, G003.1-00.6, G12.75-0.15, G35.40-1.80, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We examined the latest data release from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey covering 345° < l < 60° and 180° < l < 240°, using these data and that of the Widefield Infrared Survey Explorer to follow up proposed candidate Supernova Remnant (SNR) from other sources. Of the 101 candidates proposed in the region, we are able to definitively confirm ten as SNRs, tentatively confirm two as SNRs, and reclassify five as H uc(ii) regions. A further two are detectable in our images but difficult to classify; the remaining 82 are undetectable in these data. We also investigated the 18 unclassified Multi-Array Galactic Plane Imaging Survey (MAGPIS) candidate SNRs, newly confirming three as SNRs, reclassifying two as H uc(ii) regions, and exploring the unusual spectra and morphology of two others.

Published
2019

5. A first glimpse at the Galactic plane with the ASKAP: the SCORPIO field.

Author

Umana, G, Trigilio, C, Ingallinera, A, Riggi, S, Cavallaro, F, Marvil, J, Norris, R P, Hopkins, A M, Buemi, C S, Bufano, F, Leto, P, Loru, S, Bordiu, C, Bunton, J D, Collier, J D, Filipovic, M, Franzen, T M O, Thompson, M A, Andernach, H, and Carretti, E

Subjects
SUPERNOVA remnants, PLANETARY nebulae, STELLAR evolution, STAR formation, IMAGE processing
Abstract

In the broad context of the Australian Square Kilometer Array Pathfinder (ASKAP) early-science phase and preparation for the related surveys, we report the first radio observations towards the Galactic plane. The targeted field was chosen to encompass the entire SCORPIO survey, one of the several pathfinder projects for the Evolutionary Map of the Universe survey planned with the ASKAP. The observations were carried out in 2018 January at a central frequency of 912 MHz, with 15 operational antennas, and covered a total area of about 40 square degrees in three different pointings. The final image has a resolution of 24.1 × 21.1 arcsec2 and a median rms of |$541\ \mu \mathrm{Jy\ beam}^{-1}$|⁠. We were able to extract 3545 candidate sources, 75 per cent of them point sources. For a preliminary validation, a comparison with the 843 MHz Molonglo Galactic Plane Survey is presented. Although the present observations were obtained with the ASKAP only partially deployed, its unique capability to map complex sources, such as those inhabiting the Galactic plane, at different angular scales, is highlighted. Within the SCORPIO field all the previously classified H  ii regions, Planetary Nebulae (PNe), and supernovae remnants (SNRs), previously known to be radio sources, were detected. We also report new radio detections from several H  ii regions previously classified as 'candidates' or 'radio quiet' and from half of all the PNe in the SCORPIO field with robust classification. Most notably, we find numerous unclassified, extended sources which constitute a promising sample of candidates H  ii regions and SNRs. [ABSTRACT FROM AUTHOR]

Published
2021
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6. A Serendipitous MWA Search for Narrow-band and Broad-band Low Frequency Radio Transmissions from 1I/2017 U1 'Oumuamua

Author

Tingay, S. J., Kaplan, D. L., Lenc, E., Croft, S., McKinley, B., Beardsley, A., Crosse, B., Emrich, D., Franzen, T. M. O., Gaensler, B. M., Horsley, L., Johnston-Hollitt, M., Kenney, D., Morales, M. F., Pallot, D., Steele, K., Trott, C. M., Walker, M., Wayth, R. B., Williams, A., and Wu, C.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract

We examine data from the Murchison Widefield Array (MWA) in the frequency range 72 -- 102 MHz for a field-of-view that serendipitously contained the interstellar object 'Oumuamua on 2017 November 28. Observations took place with time resolution of 0.5 s and frequency resolution of 10 kHz. %This observation was undertaken for another purpose but due to the MWA's extremely large field-of-view, 'Oumuamua was serendipitously observed simultaneously. Based on the interesting but highly unlikely suggestion that 'Oumuamua is an interstellar spacecraft, due to some unusual orbital and morphological characteristics, we examine our data for signals that might indicate the presence of intelligent life associated with 'Oumuamua. We searched our radio data for: 1) impulsive narrow-band signals; 2) persistent narrow-band signals; and 3) impulsive broadband signals. We found no such signals with non-terrestrial origins and make estimates of the upper limits on Equivalent Isotropic Radiated Power (EIRP) for these three cases of approximately 7 kW, 840 W, and 100 kW, respectively. These transmitter powers are well within the capabilities of human technologies, and are therefore plausible for alien civilizations. While the chances of positive detection in any given Search for Extraterrestrial Intelligence (SETI) experiment are vanishingly small, the characteristics of new generation telescopes such as the MWA (and in the future, the Square Kilometre Array) make certain classes of SETI experiment easy, or even a trivial by-product of astrophysical observations. This means that the future costs of SETI experiments are very low, allowing large target lists to partially balance the low probability of a positive detection., Nine pages, four figures. Accepted for publication in ApJ

Published
2018

7. Spectral variability of radio sources at low frequencies.

Author

Ross, K, Callingham, J R, Hurley-Walker, N, Seymour, N, Hancock, P, Franzen, T M O, Morgan, J, White, S V, Bell, M E, and Patil, P

Subjects
RADIO galaxies, RADIO interferometers, RADIO sources (Astronomy), RADIOS, ACTINIC flux, INFORMATION resources
Abstract

Spectral variability of radio sources encodes information about the conditions of intervening media, source structure, and emission processes. With new low-frequency radio interferometers observing over wide fractional bandwidths, studies of spectral variability for a large population of extragalactic radio sources are now possible. Using two epochs of observations from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey that were taken one year apart, we search for spectral variability across 100–230 MHz for 21 558 sources. We present methodologies for detecting variability in the spectrum between epochs and for classifying the type of variability: either as a change in spectral shape or as a uniform change in flux density across the bandwidth. We identify 323 sources with significant spectral variability over a year-long time-scale. Of the 323 variable sources, we classify 51 of these as showing a significant change in spectral shape. Variability is more prevalent in peaked-spectrum sources, analogous to gigahertz-peaked spectrum and compact steep-spectrum sources, compared to typical radio galaxies. We discuss the viability of several potential explanations of the observed spectral variability, such as interstellar scintillation and jet evolution. Our results suggest that the radio sky in the megahertz regime is more dynamic than previously suggested. [ABSTRACT FROM AUTHOR]

Published
2021
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8. Searching for dark matter signals from local dwarf spheroidal galaxies at low radio frequencies in the GLEAM survey.

Author

Cook, R H W, Seymour, N, Spekkens, K, Hurley-Walker, N, Hancock, P J, Bell, M E, Callingham, J R, For, B-Q, Franzen, T M O, Gaensler, B M, Hindson, L, Johnston-Hollitt, M, Kapińska, A D, Morgan, J, Offringa, A R, Procopio, P, Staveley-Smith, L, Wayth, R B, Wu, C, and Zheng, Q

Subjects
ELLIPTICAL galaxies, DWARF galaxies, DARK matter, WEAKLY interacting massive particles, RADIO frequency, RADIO galaxies
Abstract

The search for emission from weakly interacting massive particle (WIMP) dark matter annihilation and decay has become a multipronged area of research not only targeting a diverse selection of astrophysical objects, but also taking advantage of the entire electromagnetic spectrum. The decay of WIMP particles into standard model particles has been suggested as a possible channel for synchrotron emission to be detected at low radio frequencies. Here, we present the stacking analysis of a sample of 33 dwarf spheroidal (dSph) galaxies with low-frequency (72–231 MHz) radio images from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey. We produce radial surface brightness profiles of images centred upon each dSph galaxy with background radio sources masked. We remove 10 fields from the stacking due to contamination from either poorly subtracted, bright radio sources or strong background gradients across the field. The remaining 23 dSph galaxies are stacked in an attempt to obtain a statistical detection of any WIMP-induced synchrotron emission in these systems. We find that the stacked radial brightness profile does not exhibit a statistically significant detection above the 95 per cent confidence level of ∼1.5 mJy beam−1. This novel technique shows the potential of using low-frequency radio images to constrain fundamental properties of particle dark matter. [ABSTRACT FROM AUTHOR]

Published
2020
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10. Supplement: 'Localization and Broadband Follow-up of the Gravitational-wave Transient GW150914' (2016, ApJS, 225, 8)

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Bodiya, T. P., Goetz, R., Mihara, T., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Miao, H., Gossan, S. E., Walsh, S., Johnson, M. D., Aston, S. M., Tomida, H., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Wang, G., Michel, C., Gray, C., Greco, G., Ueno, S., Johnson, M. W. G., Green, A. C., Astone, P., Groot, P., Grote, H., Grunewald, S., Vikram, V., Guidi, G. M., Guo, X., Nichol, R. C., Gupta, A., Tsunemi, H., Gupta, M. K., Gushwa, K. E., Karliner, I., Gustafson, E. K., Gustafson, R., Wang, H., Aufmuth, P., Hacker, J. J., Hall, B. R., Hall, E. D., Middleton, H., Cavalier, F., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Wang, M., Braginsky, V. B., Hanna, C., Hannam, M. D., Hanson, J., Aulbert, C., Hardwick, T., Cowperthwaite, P. S., Mikhailov, E. E., Haris, K., Harms, J., Wang, X., Harry, G. M., Harry, I. W., Hart, M. J., Kasen, D., Hartman, M. T., Haster, C. -J., Haughian, K., Matsuoka, M., Heidmann, A., Milano, L., Wang, Y., Babak, S., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Kent, S., Heng, I. S., MAXI Collaboration, Hennig, J., Ward, R. L., Heptonstall, A. W., Miller, J., Heurs, M., Hild, S., Bacon, P., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Mason, K., Warner, J., Kessler, R., Holt, K., Holz, D. E., Millhouse, M., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Bader, M. K. M., Howell, E. J., Smith, M., Fraser, M., Croft, S., Hu, Y. M., Huang, S., Kim, A. G., Huerta, E. A., Królak, A., Batch, J. C., Huet, D., Hughey, B., Husa, S., Martini, P., Huttner, S. H., Feng, L., Huynh-Dinh, T., Idrisy, A., Baker, P. T., Indik, N., Ingram, D. R., Carrasco Kind, M., Minenkov, Y., Inta, R., Was, M., Isa, H. N., Isac, J. -M., Franzen, T. M. O., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Baldaccini, F., Jacqmin, T., Weaver, B., Ming, J., Kuehn, K., Jang, H., Gaensler, B. M., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Boer, M., Jones, R., Jonker, R. J. G., Mirshekari, S., Ballardin, G., Johnston-Hollitt, M., Kuropatkin, N., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Wei, L. -W., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Mishra, C., Kaplan, D. L., Katsavounidis, E., Katzman, W., Lahav, O., Ballmer, S. W., Walker, A. R., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Morales, M. F., Nord, B., Keitel, D., Kelley, D. B., Weinert, M., Kells, W., Li, T. S., Kennedy, R., Barayoga, J. C., Key, J. S., Khalaidovski, A., Khalili, F. Y., Tingay, S. J., Khan, I., Mitra, S., Weinstein, A. J., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Lima, M., Kim, C., Kim, J., Barclay, S. E., Crocce, M., Kim, K., Weiss, R., Kim, N., Mitrofanov, V. P., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Branchesi, M., Kleybolte, L., Cavalieri, R., Blackburn, J. K., Welborn, T., Klimenko, S., Koehlenbeck, S. M., Barish, B. C., Mitselmakher, G., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Martin, R. M., Masserot, A., Mittleman, R., Barker, D., Moggi, A., Mohan, M., Baune, C., Mohapatra, S. R. P., Montani, M., Moore, B. C., Nugent, P., Matone, L., Moore, C. J., Wayth, R. B., Moraru, D., Moreno, G., Krueger, C., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Bavigadda, V., Wen, L., Mueller, C. L., Mueller, G., Williams, A., Ogando, R., Muir, A. W., Mukherjee, A., Kuehn, G., Mukherjee, D., Mukherjee, S., Mukund, N., Lord, J. E., Mullavey, A., Munch, J., Murphy, D. J., Murchison Wide-field Array (MWA Collaboration), Bazzan, M., Murray, P. G., Petravick, D., Mytidis, A., Kumar, P., Nardecchia, I., Wessels, P., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Smartt, S. J., Nelemans, G., Neri, M., Neunzert, A., Behnke, B., Plazas, A. A., Westphal, T., Kuo, L., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Chambers, K. C., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Wette, K., Nuttall, L. K., Oberling, J., Kutynia, A., Quataert, E., Bejger, M., Ochsner, E., Smith, K. W., O'Dell, J., Oelker, E., Ogin, G. H., Whelan, J. T., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Maia, M. A. G., Oppermann, P., Roe, N., Huber, M. E., Oram, R. J., Bell, A. S., Bogaert, G., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Lackey, B. D., Pai, A., Young, D. R., Pai, S. A., Thorne, K. S., Allen, W. H., Fernández-Muñoz, R., Romer, A. K., Palamos, J. R., Palashov, O., Bell, C. J., Palliyaguru, N., Palomba, C., Pal-Singh, A., Landry, M., Wright, D. E., Wechsler, R. H., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Affeldt, C., Paoletti, F., Paoli, A., Papa, M. A., Berger, B. K., Paris, H. R., White, D. J., Cunha, C. E., Lange, J., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Briant, T., Patricelli, B., Patrick, Z., Inserra, C., Pearlstone, B. L., Massinger, T. J., Pedraza, M., Lantz, B., Bergman, J., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Whiting, B. F., Roodman, A., Phelps, M., Schultz, A., Piccinni, O., Pichot, M., Lasky, P. D., Piergiovanni, F., Pierro, V., Bergmann, G., Pillant, G., Williams, R. D., Pinard, L., Pinto, I. M., Pitkin, M., Cella, G., Rosell, A. C., Poggiani, R., Popolizio, P., Barone, F., Post, A., Powell, J., Lorenzini, M., Prasad, J., Predoi, V., Berry, C. P. L., Premachandra, S. S., Denneau, L., Prestegard, T., Price, L. R., Rykoff, E. S., Prijatelj, M., Lazzarini, A., Williamson, A. R., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Flewelling, H., Punturo, M., Bersanetti, D., Puppo, P., Pürrer, M., Willis, J. L., Sako, M., Lazzaro, C., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Magnier, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Willke, B., Radkins, H., Bertolini, A., Raffai, P., Leaci, P., Sanchez, E., Raja, S., Rakhmanov, M., Primak, N., Rapagnani, P., Raymond, V., Levine, B. M., Wimmer, M. H., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Leavey, S., Betzwieser, J., Scarpine, V., Rest, A., Rei, L., Winkler, W., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Margutti, R., Robie, R., Sherstyuk, A., Wipf, C. C., Robinet, F., Schindler, R., Bhagwat, S., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Lebigot, E. O., Wittel, H., Stalder, B., Romie, J. H., Rosińska, D., Rowan, S., Yock, P. C., Schubnell, M., Rüdiger, A., Bhandare, R., Ruggi, P., Ryan, K., Kankare, E., Sachdev, S., Stubbs, C. W., Lee, C. H., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Scolnic, D., Samajdar, A., Wester, W., Sammut, L., Bilenko, I. A., Masso-Reid, M., Sanchez, E. J., Lee, H. K., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Bogan, C., Saulson, P. R., Sevilla-Noarbe, I., Sauter, O., D'Andrea, C. B., Savage, R. L., Sawadsky, A., Lee, H. M., Billingsley, G., Schale, P., Schilling, R., Woan, G., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Tonry, J., Brillet, A., Schönbeck, A., Schreiber, E., Lee, K., Schuette, D., Loriette, V., Schutz, B. F., Birch, J., Scott, J., Scott, S. M., Sellers, D., Waters, C., Sentenac, D., Sequino, V., Sheldon, E., Sergeev, A., Worden, J., Lenon, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Birney, R., Cepeda, C. B., Shah, S., Shahriar, M. S., Shaltev, M., Thrane, E., Wright, J. 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Abstract

This Supplement provides supporting material for Abbott et al. (2016a). We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands.

Published
2016

11. Study of the galactic radio sources in the SCORPIO survey resolved by ATCA at 2.1 GHz.

Author

Ingallinera, A, Umana, G, Trigilio, C, Norris, R, Franzen, T M O, Cavallaro, F, Leto, P, Buemi, C, Schillirò, F, Bufano, F, Riggi, S, Loru, S, and Agliozzo, C

Subjects
PLANETARY nebulae, SUPERNOVA remnants, WOLF-Rayet stars, VARIABLE stars, RADIOS, STELLAR evolution
Abstract

We present a catalogue of a large sample of extended radio sources in the Stellar Continuum Originating from Radio Physics In Ourgalaxy (SCORPIO) field, observed and resolved by the Australia Telescope Compact Array. SCORPIO, a pathfinder project for addressing the early operations of the Australia SKA Pathfinder, is a survey of ∼5 square degrees between 1.4 and 3.1 GHz, centred at l  = 343.5°, b  = 0.75°, and with an angular resolution of about 10 arcsec. It is aimed at understanding the scientific and technical challenges to be faced by future Galactic surveys. With a mean sensitivity around |$100\ \mu \mathrm{Jy\ beam}^{-1}$| and the possibility to recover angular scales at least up to 4 arcmin, we extracted 99 extended sources, 35 of them detected for the first time. Among the 64 known sources 55 had at least a tentative classification in literature. Studying the radio morphology and comparing the radio emission with infrared we propose as candidates six new H  ii regions, two new planetary nebulae, two new luminous blue variable or Wolf–Rayet stars, and three new supernova remnants. This study provides an overview of the potentiality of future radio surveys in terms of Galactic source extraction and characterization and a discussion on the difficulty to reduce and analyse interferometric data on the Galactic plane. [ABSTRACT FROM AUTHOR]

Published
2019
Full Text
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13. Interplanetary scintillation studies with the Murchison Widefield Array III: comparison of source counts and densities for radio sources and their sub-arcsecond components at 162 MHz.

Author

Chhetri, R, Ekers, R D, Morgan, J, Macquart, J-P, and Franzen, T M O

Subjects
INTERPLANETARY medium, SCINTILLATORS, SPECTRAL energy distribution, ASTRONOMICAL observations, RADIO sources (Astronomy), GALACTIC evolution
Abstract

We use Murchison Widefield Array (MWA) observations of interplanetary scintillation (IPS) to determine the source counts of point (<0.3 arcsec extent) sources and of all sources with some subarcsecond structure, at 162 MHz. We have developed the methodology to derive these counts directly from the IPS observables, while taking into account changes in sensitivity across the survey area. The counts of sources with compact structure follow the behaviour of the dominant source population above ∼3 Jy but below this they show Euclidean behaviour. We compare our counts to those predicted by simulations and find a good agreement for our counts of sources with compact structure, but significant disagreement for point source counts. Using low radio frequency spectral energy distributions (SEDs) from the Galactic and Extragalactic MWA survey, we classify point sources as compact steep spectrum (CSS), flat spectrum, or peaked. If we consider the CSS sources to be the more evolved counterparts of the peaked sources, the two categories combined comprise approximately 80 per cent of the point source population. We calculate densities of potential calibrators brighter than 0.4 Jy at low frequencies and find 0.2 sources per square degrees for point sources, rising to 0.7 sources per square degree if sources with more complex arcsecond structure are included. We extrapolate to estimate 4.6 sources per square degrees at 0.04 Jy. We find that a peaked spectrum is an excellent predictor for compactness at low frequencies, increasing the number of good calibrators by a factor of three compared to the usual flat spectrum criterion. [ABSTRACT FROM AUTHOR]

Published
2018
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14. Limits on radio emission from meteors using the MWA.

Author

Zhang, X., Hancock, P., Devillepoix, H. A. R., Wayth, R. B., Beardsley, A., Crosse, B., Emrich, D., Franzen, T. M. O., Gaensler, B. M., Horsley, L., Johnston-Hollitt, M., Kaplan, D. L., Kenney, D., Morales, M. F., Pallot, D., Steele, K., Tingay, S. J., Trott, C. M., Walker, M., and Williams, A.

Subjects
ASTROPHYSICS, LONG wavelength spectrometers, METEORS, SPECTRAL analysis (Phonetics), TELESCOPES
Abstract

Recently, low-frequency, broad-band radio emission has been observed accompanying bright meteors by the Long Wavelength Array (LWA). The broad-band spectra between 20 and 60MHz were captured for several events, while the spectral index (dependence of flux density on frequency, with Sv ∝ vα) was estimated to be -4 ± 1 during the peak of meteor afterglows. Here we present a survey of meteor emission and other transient events using the Murchison Wide Field Array (MWA) at 72-103MHz. In our 322 h survey, down to a 5σ detection threshold of 3.5 Jy beam-1, no transient candidates were identified as intrinsic emission from meteors. We derived an upper limit of -3.7 (95 per cent confidence limit) on the spectral index in our frequency range. We also report detections of other transient events, such as reflected FM broadcast signals from small satellites, conclusively demonstrating the ability of the MWA to detect and track space debris on scales as small as 0.1 m in low Earth orbits. [ABSTRACT FROM AUTHOR]

Published
2018
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15. SCORPIO – II. Spectral indices of weak Galactic radio sources.

Author

Cavallaro, F., Trigilio, C., Umana, G., Franzen, T. M. O., Norris, R. P., Leto, P., Ingallinera, A., Buemi, C. S., Marvil, J., Agliozzo, C., Bufano, F., Cerrigone, L., and Riggi, S.

Subjects
GALAXIES, RADIO astronomy, INTERSTELLAR medium, PLANETARY nebulae, RADIO sources (Astronomy)
Abstract

In the next few years the classification of radio sources observed by the large surveys will be a challenging problem and spectral index is a powerful tool for addressing it. Here we present an algorithm to estimate the spectral index of sources from multiwavelength radio images. We have applied our algorithm to SCORPIO, a Galactic plane survey centred around 2.1 GHz carried out with Australian Telescope Compact Array and found we can measure reliable spectral indices only for sources stronger than 40 times the rms noise. Above a threshold of 1 mJy, the source density in SCORPIO is 20 per cent greater than in a typical extragalactic field, like Australia Telescope Large Area Survey because of the presence of Galactic sources. Among this excess population, 16 sources per square degree have a spectral index of about zero suggesting optically thin thermal emission such as H II regions and planetary nebulae, while 12 per square degree present a rising spectrum, suggesting optically thick thermal emission such as stars and UCH II regions. [ABSTRACT FROM AUTHOR]

Published
2018
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16. The Phase II Murchison Widefield Array: Design overview.

Author

Wayth, Randall B., Tingay, Steven J., Trott, Cathryn M., Emrich, David, Johnston-Hollitt, Melanie, McKinley, Ben, Gaensler, B. M., Beardsley, A. P., Booler, T., Crosse, B., Franzen, T. M. O., Horsley, L., Kaplan, D. L., Kenney, D., Morales, M. F., Pallot, D., Sleap, G., Steele, K., Walker, M., and Williams, A.

Published
2018
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17. In situ measurement of MWA primary beam variation using ORBCOMM.

Author

Line, J. L. B., McKinley, B., Rasti, J., Bhardwaj, M., Wayth, R. B., Webster, R. L., Ung, D., Emrich, D., Horsley, L., Beardsley, A., Crosse, B., Franzen, T. M. O., Gaensler, B. M., Johnston-Hollitt, M., Kaplan, D. L., Kenney, D., Morales, M. F., Pallot, D., Steele, K., and Tingay, S. J.

Published
2018
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18. 30 GHz observations of sources in the VSA fields

Author

Gawronski, M. P., Peel, M. W., Lancaster, K., Battye, R. A., Birkinshaw, M., Browne, I. W. A., Davies, M. L., Davis, R. J., Feiler, R., Franzen, T. M. O., Genova-Santos, R., Kus, A. J., Lowe, S. R., Pazderska, B. M., Pazderski, E., Pooley, G. G., Roukema, B. F., Waldram, E. M., and Wilkinson, P. N.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Small angular scale (high l) studies of cosmic microwave background anisotropies require accurate knowledge of the statistical properties of extragalactic sources at cm-mm wavelengths. We have used a 30 GHz dual-beam receiver (OCRA-p) on the Torun 32-m telescope to measure the flux densities of 121 sources in VSA fields selected at 15 GHz with the Ryle Telescope. We have detected 57 sources above a limiting flux density of 5mJy, of which 31 sources have a flux density greater than 10mJy, which is our effective completeness limit. From these measurements we derive a surface density of sources above 10mJy at 30 GHz of 2.0+/-0.4 per square degree. This is consistent with the surface density obtained by Mason et al. (2009) who observed a large sample of sources selected at a much lower frequency (1.4 GHz). We have also investigated the dependence of the spectral index distribution on flux density by comparing our results with those for sources above 1 Jy selected from the WMAP 22 GHz catalogue. We conclude that the proportion of steep spectrum sources increases with decreasing flux density, qualitatively consistent with the predictions of deZotti et al. (2005). We find no evidence for an unexpected population of sources whose spectra rise towards high frequencies, which would affect our ability to interpret current high resolution CMB observations at 30 GHz and above., 12 pages, 12 figures, submitted to MNRAS

Published
2009

19. GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey -- I. A low-frequency extragalactic catalogue.

Author

Hurley-Walker, N., Callingham, J. R., Hancock, P. J., Franzen, T. M. O., Hindson, L., Kapinska, A. D., Morgan, J., Offringa, A. R., Wayth, R. B., Wu, C., Zheng, Q., Murphy, T., Bell, M. E., Dwarakanath, K. S., For, B., Gaensler, B. M., Johnston-Hollitt, M., Lenc, E., Procopio, P., and Staveley-Smith, L.

Subjects
EXTRAGALACTIC distances, ASTRONOMICAL surveys, MAGELLANIC clouds, ACTINIC flux, METAPHYSICAL cosmology
Abstract

Using the Murchison Widefield Array (MWA), the low-frequency Square Kilometre Array precursor located in Western Australia, we have completed the GaLactic and Extragalactic All-sky MWA (GLEAM) survey, and present the resulting extragalactic catalogue, utilizing the first year of observations. The catalogue covers 24 831 square degrees, over declinations south of +30° and Galactic latitudes outside 10° of the Galactic plane, excluding some areas such as the Magellanic Clouds. It contains 307 455 radio sources with 20 separate flux density measurements across 72-231 MHz, selected from a time- and frequency-integrated image centred at 200 MHz, with a resolution of ≈2 arcmin. Over the catalogued region, we estimate that the catalogue is 90 per cent complete at 170 mJy, and 50 per cent complete at 55 mJy, and large areas are complete at even lower flux density levels. Its reliability is 99.97 per cent above the detection threshold of 5s, which itself is typically 50 mJy. These observations constitute the widest fractional bandwidth and largest sky area survey at radio frequencies to date, and calibrate the low-frequency flux density scale of the southern sky to better than 10 per cent. This paper presents details of the flagging, imaging, mosaicking and source extraction/characterization, as well as estimates of the completeness and reliability. All source measurements and images are available online. 1 This is the first in a series of publications describing the GLEAM survey results. [ABSTRACT FROM AUTHOR]

Published
2017
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22. Low radio frequency observations and spectral modelling of the remnant of Supernova 1987A.

Author

Callingham, J. R., Gaensler, B. M., Zanardo, G., Staveley-Smith, L., Hancock, P. J., Hurley-Walker, N., Bell, M. E., Dwarakanath, K. S., Franzen, T. M. O., Hindson, L., Johnston-Hollitt, M., Kapińska, A., For, B.-Q., Lenc, E., McKinley, B., Morgan, J., Offringa, A. R., Procopio, P., Wayth, R. B., and Wu, C.

Subjects
ASTRONOMICAL observations, CIRCUMSTELLAR matter, SUPERNOVA remnants, RADIO frequency, SPECTRUM analysis
Abstract

We present Murchison Widefield Array observations of the supernova remnant (SNR) 1987A between 72 and 230 MHz, representing the lowest frequency observations of the source to date. This large lever arm in frequency space constrains the properties of the circumstellar medium created by the progenitor of SNR 1987A when it was in its red supergiant phase. As of late 2013, the radio spectrum of SNR 1987A between 72 MHz and 8.64 GHz does not show any deviation from a non-thermal power law with a spectral index of -0.74 ± 0.02. This spectral index is consistent with that derived at higher frequencies, beneath 100 GHz, and with a shock in its adiabatic phase. A spectral turnover due to free-free absorption by the circumstellar medium has to occur below 72 MHz, which places upper limits on the optical depth of ≤0.1 at a reference frequency of 72 MHz, emission measure of≲13 000 cm-6 pc, and an electron density of ≲110 cm-3. This upper limit on the electron density is consistent with the detection of prompt radio emission and models of the X-ray emission from the supernova. The electron density upper limit implies that some hydrodynamic simulations derived a red supergiant mass-loss rate that is too high, or a wind velocity that is too low. The mass-loss rate of ~5 × 10-6 M⊙ yr-1 and wind velocity of 10 km s-1 obtained from optical observations are consistent with our upper limits, predicting a current turnover frequency due to free-free absorption between 5 and 60 MHz. [ABSTRACT FROM AUTHOR]

Published
2016
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23. The 154 MHz radio sky observed by the Murchison Widefield Array: noise, confusion, and first source count analyses.

Author

Franzen, T. M. O., Jackson, C. A., Offringa, A. R., Ekers, R. D., Wayth, R. B., Bernardi, G., Bowman, J. D., Briggs, F., Cappallo, R. J., Deshpande, A. A., Gaensler, B. M., Greenhill, L. J., Hazelton, B. J., Johnston-Hollitt, M., Kaplan, D. L., Lonsdale, C. J., McWhirter, S. R., Mitchell, D. A., Morales, M. F., and Morgan, E.

Subjects
*ASTRONOMICAL observations, *DECONVOLUTION (Mathematics), *ASTROPHYSICS, *FLUX (Energy), *BANDWIDTHS
Abstract

We analyse a 154 MHz image made from a 12 h observation with the Murchison Widefield Array (MWA) to determine the noise contribution and behaviour of the source counts down to 30 mJy. The MWA image has a bandwidth of 30.72 MHz, a field-of-view within the halfpower contour of the primary beam of 570 deg2, a resolution of 2.3 arcmin and contains 13 458 sources above 5σ. The rms noise in the centre of the image is 4-5 mJy beam-1. The MWA counts are in excellent agreement with counts from other instruments and are the most precise ever derived in the flux density range 30-200 mJy due to the sky area covered. Using the deepest available source count data, we find that the MWA image is affected by sidelobe confusion noise at the ≈3.5 mJy beam-1 level, due to incompletely peeled and out-of-image sources, and classical confusion becomes apparent at ≈1.7 mJy beam-1. This work highlights that (i) further improvements in ionospheric calibration and deconvolution imaging techniques would be required to probe to the classical confusion limit and (ii) the shape of low-frequency source counts, including any flattening towards lower flux densities, must be determined from deeper ≈150 MHz surveys as it cannot be directly inferred from higher frequency data. [ABSTRACT FROM AUTHOR]

Published
2016
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24. 10C continued: a deeper radio survey at 15.7 GHz.

Author

Whittam, I. H., Riley, J. M., Green, D. A., Davies, M. L., Franzen, T. M. O., Rumsey, C., Schamme, M. P., and Waldram, E. M.

Subjects
STAR formation, GALAXY formation, FLUX (Energy), DENSITY of stars, STAR observations
Abstract

We present deep 15.7 GHz observations made with the Arcminute Microkelvin Imager Large Array in two fields previously observed as part of the Tenth Cambridge (10C) survey. These observations allow the source counts to be calculated down to 0.1 mJy, a factor of 5 deeper than achieved by the 10C survey. The new source counts are consistent with the extrapolated fit to the 10C source count, and display no evidence for either steepening or flattening of the counts. There is thus no evidence for the emergence of a significant new population of sources (e.g. star forming) at 15.7 GHz flux densities above 0.1 mJy, the flux density level at which we expect star-forming galaxies to begin to contribute. Comparisons with the de Zotti et al. model and the SKADS Simulated Sky show that they both underestimate the observed number of sources by a factor of 2 at this flux density level. We suggest that this is due to the flat-spectrum cores of radio galaxies contributing more significantly to the counts than predicted by the models. [ABSTRACT FROM AUTHOR]

Published
2016
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25. SCORPIO: a deep survey of radio emission from the stellar life-cycle.

Author

Umana, G., Trigilio, C., Franzen, T. M. O., Norris, R. P., Leto, P., Ingallinera, A., Buemi, C. S., Agliozzo, C., Cavallaro, F., and Cerrigone, L.

Subjects
ASTRONOMICAL observations, STELLAR evolution, SOLAR radio emission, INTERSTELLAR medium, STAR formation
Abstract

Radio emission has been detected in a broad variety of stellar objects from all stages of stellar evolution. However, most of our knowledge originates from targeted observations of small samples, which are strongly biased to sources which are peculiar at other wavelengths. In order to tackle this problem we have conducted a deep 1.4 GHz survey by using the Australian Telescope Compact Array, with a net bandwidth of 1.7 GHz (1.4-3.1 GHz), following the same observing setup as that used for the Australia Telescope Large Area Survey project, this time choosing a region more appropriate for stellar work. In this paper, the Stellar Continuum Originating from Radio Physics In Ourgalaxy (SCORPIO) project is presented as well as results from the pilot experiment. The achieved rms is 30 µJy and the angular resolution ˜10 arcsec. 614 point-like sources have been extracted just from the pilot field. Only 34 of them are classified in SIMBAD or the NASA/IPAC Extragalactic Database. About 80 per cent of the extracted sources are reported in one of the inspected catalogues and 50 per cent of them appears to belong to a reddened stellar/Galactic population. However, the evaluation of extragalactic contaminants is very difficult without further investigations. Interesting results have been obtained for extended radio sources that fall in the SCORPIO field. Many roundishlike structures (indicated as bubbles in the following) have been found, some of which are classified at other wavelengths. However, for all of these sources, our project has provided us with images of unprecedented sensitivity and angular resolution. [ABSTRACT FROM AUTHOR]

Published
2015
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26. ATLAS - I. Third release of 1.4 GHz mosaics and component catalogues.

Author

Franzen, T. M. O., Banfield, J. K., Hales, C. A., Hopkins, A., Norris, R. P., Seymour, N., Chow, K. E., Herzog, A., Huynh, M. T., Lenc, E., Mao, M. Y., and Middelberg, E.

Subjects
*ASTRONOMICAL observations, *BANDWIDTHS, *RADIO sources (Astronomy), *TELESCOPES
Abstract

We present the third data release from the Australia Telescope Large Area Survey. These data combine the observations at 1.4GHz before and after upgrades to the Australia Telescope Compact Array reaching a sensitivity of 14μJy beam-1 in 3.6 deg² over the Chandra Deep Field South (CDFS) and of 17μJy beam-1 in 2.7 deg² over the European Large Area ISO Survey South 1 (ELAIS-S1). We used a variety of array configurations to maximize the uv coverage resulting in a resolution of 16 by 7 arcsec in CDFS and of 12 by 8 arcsec in ELAIS-S1. After correcting for peak bias and bandwidth smearing, we find a total of 3034 radio source components above 5σ in CDFS, of which 514 (17 per cent) are considered to be extended. The number of components detected above 5σ in ELAIS-S1 is 2084, of which 392 (19 per cent) are classified as extended. The catalogues include reliable spectral indices (Δα < 0.2) between 1.40 and 1.71 GHz for ~350 of the brightest components. [ABSTRACT FROM AUTHOR]

Published
2015
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27. 30 GHz observations of sources in the Very Small Array fields.

Author

Gawroński, M. P., Peel, M. W., Lancaster, K., Battye, R. A., Birkinshaw, M., Browne, I. W. A., Davies, M. L., Davis, R. J., Feiler, R., Franzen, T. M. O., Génova-Santos, R., Kus, A. J., Lowe, S. R., Pazderska, B. M., Pazderski, E., Pooley, G. G., Roukema, B. F., Waldram, E. M., and Wilkinson, P. N.

Subjects
COSMIC background radiation, ASTROPHYSICAL radiation, ANISOTROPY, RADIO sources (Astronomy), SPECTRUM analysis
Abstract

Small angular scale (high ℓ) studies of cosmic microwave background (CMB) anisotropies require accurate knowledge of the statistical properties of extragalactic sources at cm-mm wavelengths. We have used a 30 GHz dual-beam receiver (One Centimetre Receiver Array prototype) on the Toruń 32-m telescope to measure the flux densities of 121 sources in Very Small Array fields selected at 15 GHz with the Ryle Telescope. We have detected 57 sources above a limiting flux density of 5 mJy, of which 31 sources have a flux density greater than 10 mJy, which is our effective completeness limit. From these measurements we derive a surface density of sources above 10 mJy at 30 GHz of deg−2. This is consistent with the surface density obtained by Mason et al. who observed a large sample of sources selected at a much lower frequency (1.4 GHz). We have also investigated the dependence of the spectral index distribution on flux density by comparing our results with those for sources above 1 Jy selected from the Wilkinson Microwave Anisotropy Probe 22 GHz catalogue. We conclude that the proportion of steep spectrum sources increases with decreasing flux density, qualitatively consistent with the predictions of de Zotti et al. We find no evidence for an unexpected population of sources above our completeness limit of 10 mJy whose spectra rise towards high frequencies, which would affect our ability to interpret current high-resolution CMB observations at 30 GHz and above. [ABSTRACT FROM AUTHOR]

Published
2010
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28. The Arcminute Microkelvin Imager.

Author

Zwart, J. T. L., Barker, R. W., Biddulph, P., Bly, D., Boysen, R. C., Brown, A. R., Clementson, C., Crofts, M., Culverhouse, T. L., Czeres, J., Dace, R. J., Davies, M. L., D'Alessandro, R., Doherty, P., Duggan, K., Ely, J. A., Felvus, M., Feroz, F., Flynn, W., and Franzen, T. M. O.

Subjects
INTERFEROMETERS, ASTRONOMICAL instruments, GALAXY clusters, OPTICAL instruments, TELESCOPES
Abstract

The Arcminute Microkelvin Imager is a pair of interferometer arrays operating with six frequency channels spanning 13.9–18.2 GHz, for observations on angular scales of 30 arcsec–10 arcmin and for declinations greater than −15°; the Small Array has a sensitivity of and the Large Array has a sensitivity of . The telescope is aimed principally at Sunyaev–Zel'dovich imaging of clusters of galaxies. We discuss the design of the telescope and describe and explain its electronic and mechanical systems. [ABSTRACT FROM AUTHOR]

Published
2008
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29. Cassiopeia A, Cygnus A, Taurus A, and Virgo A at ultra-low radio frequencies

Author

de Gasperin, F., Vink, J., McKean, J. P., Asgekar, A., Bentum, M. J., Blaauw, R., Bonafede, A., Bruggen, M., Breitling, F., Brouw, W. N., Butcher, H. R., Ciardi, B., Cuciti, V., de Vos, M., Duscha, S., Eisloffel, J., Engels, D., Fallows, R. A., Franzen, T. M. O., Garrett, M. A., Gunst, A. W., Horandel, J., Heald, G., Koopmans, L. V. E., Krankowski, A., Maat, P., Mann, G., Mevius, M., Miley, G., Nelles, A., Norden, M. J., Offringa, A. R., Orrú, E., Paas, H., Pandey-Pommier, M., Pizzo, R., Reich, W., Rowlinson, A., Schwarz, D. J., Shulevski, A., Smirnov, O., Soida, M., Tagger, M., Toribio, M. C., van Ardenne, A., van der Horst, A. J., van Haarlem, M. P., van Weeren, R. J., Vocks, C., Wucknitz, O., Zarka, P., and Zucca, P.

Subjects
13. Climate action, techniques: interferometric, radio continuum: general
Abstract

Astronomy and astrophysics 635, A150 (2020). doi:10.1051/0004-6361/201936844, Context. The four persistent radio sources in the northern sky with the highest flux density at metre wavelengths are Cassiopeia A, Cygnus A, Taurus A, and Virgo A; collectively they are called the A-team. Their flux densities at ultra-low frequencies (< 100 MHz) can reach several thousands of janskys, and they often contaminate observations of the low-frequency sky by interfering with image processing. Furthermore, these sources are foreground objects for all-sky observations hampering the study of faint signals, such as the cosmological 21 cm line from the epoch of reionisation.Aims. We aim to produce robust models for the surface brightness emission as a function of frequency for the A-team sources at ultra-low frequencies. These models are needed for the calibration and imaging of wide-area surveys of the sky with low-frequency interferometers. This requires obtaining images at an angular resolution better than 15″ with a high dynamic range and good image fidelity.Methods. We observed the A-team with the Low Frequency Array (LOFAR) at frequencies between 30 MHz and 77 MHz using the Low Band Antenna system. We reduced the datasets and obtained an image for each A-team source.Results. The paper presents the best models to date for the sources Cassiopeia A, Cygnus A, Taurus A, and Virgo A between 30 MHz and 77 MHz. We were able to obtain the aimed resolution and dynamic range in all cases. Owing to its compactness and complexity, observations with the long baselines of the International LOFAR Telescope will be required to improve the source model for Cygnus A further., Published by EDP Sciences, Les Ulis

30. LOFAR 144-MHz follow-up observations of GW170817

Author

Broderick, J. W., Shimwell, T. W., Gourdji, K., Rowlinson, A., Nissanke, S., Hotokezaka, K., Jonker, P. G., Tasse, C., Hardcastle, M. J., Oonk, J. B. R., Fender, R. P., Wijers, R. A. M. J., Shulevski, A., Stewart, A. J., Veen, S. Ter, Moss, V. A., Van Der Wiel, M. H. D., Nichols, D. A., Piette, A., Bell, M. E., Carbone, D., Corbel, S., Eislöffel, J., Grießmeier, J.-M., Keane, E. F., Law, C. J., Muñoz-Darias, T., Pietka, M., Serylak, M., Van Der Horst, A. J., Van Leeuwen, J., Wijnands, R., Zarka, P., Anderson, J. M., Bentum, M. J., Blaauw, R., Brouw, W. N., Bruggen, M., Ciardi, B., De Vos, M., Duscha, S., Fallows, R. A., Franzen, T. M. O., Garrett, M. A., Gunst, A. W., Hoeft, M., Hörandel, J. R., Iacobelli, M., Jutte, E., Koopmans, L. V. E., Krankowski, A., Maat, P., Mann, G., Mulder, H., Nelles, A., Paas, H., Pandey-Pommier, M., Pekal, R., Reich, W., Röttgering, H. J. A., Schwarz, D. J., Smirnov, O., Soida, M., Toribio, M. C., Van Haarlem, M. P., Van Weeren, R. J., Vocks, C., Wucknitz, O., and Zucca, P.

Subjects
14. Life underwater
Abstract

Monthly notices of the Royal Astronomical Society 494(4), 5110 - 5117 (2020). doi:10.1093/mnras/staa950, We present low-radio-frequency follow-up observations of AT 2017gfo, the electromagnetic counterpart of GW170817, which was the first binary neutron star merger to be detected by Advanced LIGO-Virgo. These data, with a central frequency of 144 MHz, were obtained with LOFAR, the Low-Frequency Array. The maximum elevation of the target is just 13.7 degrees when observed with LOFAR, making our observations particularly challenging to calibrate and significantly limiting the achievable sensitivity. On time-scales of 130-138 and 371-374 days after the merger event, we obtain 3$\sigma$ upper limits for the afterglow component of 6.6 and 19.5 mJy beam$^{-1}$, respectively. Using our best upper limit and previously published, contemporaneous higher-frequency radio data, we place a limit on any potential steepening of the radio spectrum between 610 and 144 MHz: the two-point spectral index $\alpha^{610}_{144} \gtrsim -2.5$. We also show that LOFAR can detect the afterglows of future binary neutron star merger events occurring at more favourable elevations., Published by Oxford Univ. Press, Oxford

31. The ASKAP/EMU Source Finding Data Challenge.

Author

Hopkins, A. M., Whiting, M. T., Seymour, N., Chow, K. E., Norris, R. P., Bonavera, L., Breton, R., Carbone, D., Ferrari, C., Franzen, T. M. O., Garsden, H., González-Nuevo, J., Hales, C. A., Hancock, P. J., Heald, G., Herranz, D., Huynh, M., Jurek, R. J., López-Caniego, M., and Massardi, M.

Published
2015
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32. GLEAM: The GaLactic and Extragalactic All-Sky MWA Survey.

Author

Wayth, R. B., Lenc, E., Bell, M. E., Callingham, J. R., Dwarakanath, K. S., Franzen, T. M. O., For, B.-Q., Gaensler, B., Hancock, P., Hindson, L., Hurley-Walker, N., Jackson, C. A., Johnston-Hollitt, M., Kapińska, A. D., McKinley, B., Morgan, J., Offringa, A. R., Procopio, P., Staveley-Smith, L., and Wu, C.

Published
2015
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34. LOCALIZATION AND BROADBAND FOLLOW-UP OF THE GRAVITATIONAL-WAVE TRANSIENT GW 150914

Author

Abbott1, B. P., Abbott1, R., Abbott2, T. D., Abernathy1, M. R., Acernese3, F., 4, Ackley5, K., Adams6, C., Adams7, T., Addesso3, P., Adhikari1, R. X., Adya8, V. B., Affeldt8, C., Agathos9, M., Agatsuma9, K., Aggarwal10, N., Aguiar11, O. D., Aiello12, L., Ain14, A., Ajith15, P., Allen8, B., 17, 16, Allocca18, A., Altin20, P. A., Anderson1, S. B., Anderson16, W. G., Arai1, K., Araya1, M. C., Arceneaux21, C. C., Areeda22, J. S., Arnaud23, N., Arun24, K. G., Ascenzi13, S., Ashton26, G., Ast27, M., Aston6, S. M., Astone28, P., Aufmuth8, P., Aulbert8, C., Babak29, S., Bacon30, P., Bader9, M. K. M., Baker31, P. T., Baldaccini32, F., Ballardin34, G., Ballmer35, S. W., Barayoga1, J. C., Barclay36, S. E., Barish1, B. C., Barker37, D., Barone3, F., Barr36, B., Barsotti10, L., Barsuglia30, M., Barta38, D., Barthelmy39, S., Bartlett37, J., Bartos40, I., Bassiri41, R., Basti18, A., Batch37, J. C., Baune8, C., Bavigadda34, V., Bazzan42, M., Behnke29, B., Bejger44, M., Bell36, A. S., Bell36, C. J., Berger1, B. K., Bergman37, J., Bergmann8, G., Berry45, C. P. L., Bersanetti46, D., Bertolini9, A., Betzwieser6, J., Bhagwat35, S., Bhandare48, R., Bilenko49, I. A., Billingsley1, G., Birch6, J., Birney50, R., Biscans10, S., Bisht8, A., Bitossi34, M., Biwer35, C., Bizouard23, M. A., Blackburn1, J. K., Blair51, C. D., Blair51, D. G., Blair37, R. M., Bloemen52, S., Bock8, O., Bodiya10, T. P., Boer53, M., Bogaert53, G., Bogan8, C., Bohe29, A., Bojtos54, P., Bond45, C., Bondu55, F., Bonnand7, R., Boom9, B. A., Bork1, R., Boschi18, V., Bose14, S., Bouffanais30, Y., Bozzi34, A., Bradaschia19, C., Brady16, P. R., Braginsky49, V. B., Branchesi57, M., Brau59, J. E., Briant60, T., Brillet53, A., Brinkmann8, M., Brisson23, V., Brockill16, P., Brooks1, A. F., Brown35, D. A., Brown45, D. D., Brown10, N. M., Buchanan2, C. C., Buikema10, A., Bulik61, T., Bulten9, H. J., Buonanno29, A., Buskulic7, D., Buy30, C., Byer41, R. L., Cadonati64, L., Cagnoli65, G., Cahillane1, C., Bustillo64, J. C., Callister1, T., Calloni4, E., Camp39, J. B., Cannon69, K. C., Cao70, J., Capano8, C. D., Capocasa30, E., Carbognani34, F., Caride71, S., Diaz23, J. C., Casentini13, C., Caudill16, S., Cavagliá21, M., Cavalier23, F., Cavalieri34, R., Cella19, G., Cepeda1, C. B., Baiardi57, L. C., Cerretani18, G., Cesarini13, E., Chakraborty1, R., Chalermsongsak1, T., Chamberlin72, S. J., Chan36, M., Chao73, S., Charlton74, P., Chassande Mottin30, E., Chen75, H. Y., Chen76, Y., Cheng73, C., Chincarini47, A., Chiummo34, A., Cho77, H. S., Cho63, M., Chow20, J. H., Christensen78, N., Chu51, Q., Chua60, S., Chung51, S., Ciani5, G., Clara37, F., Clark64, J. A., Cleva53, F., Coccia12, E., 25, 13, Cohadon60, P. F., Colla28, A., Collette80, C. G., Cominsky81, L., M. Constancio J. r., 11, Conte28, A., Conti43, L., Cook37, D., Corbitt2, T. R., Cornish31, N., Corsi71, A., Cortese34, S., Costa11, C. A., Coughlin78, M. W., Coughlin82, S. B., Coulon53, J. P., Countryman40, S. T., Couvares1, P., Cowan64, E. E., Coward51, D. M., Cowart6, M. J., Coyne1, D. C., Coyne71, R., Craig36, K., Creighton16, J. D. E., Cripe2, J., Crowder83, S. G., Cumming36, A., Cunningham36, L., Cuoco34, E., Dal Canton8, T., Danilishin36, S. L., D'Antonio13, S., Danzmann8, K., Darman84, N. S., Dattilo34, V., Dave48, I., Daveloza85, H. P., Davier23, M., Davies36, G. S., Daw86, E. J., Day34, R., Debra41, D., Debreczeni38, G., Degallaix66, J., De Laurentis4, M., Deléglise60, S., Del Pozzo45, W., Denker8, T., Dent8, T., Dereli53, H., Dergachev1, V., Derosa6, R. T., De Rosa4, R., Desalvo87, R., Dhurandhar14, S., Díaz85, M. C., Di Fiore4, L., Di Giovanni28, M., Di Lieto18, A., Di Pace28, S., Di Palma8, I., Di Virgilio19, A., Dojcinoski88, G., Dolique66, V., Donovan10, F., Dooley21, K. L., Doravari6, S., 8, Douglas36, R., Downes16, T. P., Drago8, M., 90, 89, Drever1, R. W. P., Driggers37, J. C., Du70, Z., Ducrot7, M., Dwyer37, S. E., Edo86, T. B., Edwards78, M. C., Effler6, A., Eggenstein8, H. B., Ehrens1, P., Eichholz5, J., Eikenberry5, S. S., Engels76, W., Essick10, R. C., Etzel1, T., Evans10, M., Evans6, T. M., Everett72, R., Factourovich40, M., Fafone12, V., Fair35, H., Fairhurst91, S., Fan70, X., Fang51, Q., Farinon47, S., Farr75, B., Farr45, W. M., Favata88, M., Fays91, M., Fehrmann8, H., Fejer41, M. M., Ferrante18, I., Ferreira11, E. C., Ferrini34, F., Fidecaro18, F., Fiori34, I., Fiorucci30, D., Fisher35, R. P., Flaminio66, R., Fletcher36, M., Fournier53, J. D., Franco23, S., Frasca28, S., Frasconi19, F., Frei54, Z., Freise45, A., Frey59, R., Frey23, V., Fricke8, T. T., Fritschel10, P., Frolov6, V. V., Fulda5, P., Fyffe6, M., Gabbard21, H. A. G., Gair93, J. R., Gammaitoni32, L., Gaonkar14, S. G., Garufi4, F., Gatto30, A., Gaur94, G., Gehrels39, N., Gemme47, G., Gendre53, B., Genin34, E., Gennai19, A., George48, J., Gergely96, L., Germain7, V., Ghosh15, A., Ghosh9, S., Giaime2, J. A., 6, Giardina6, K. D., Giazotto19, A., Gill97, K., Glaefke36, A., Goetz98, E., Goetz5, R., Gondan54, L., González2, G., Castro18, J. M. G., Gopakumar99, A., Gordon36, N. A., Gorodetsky49, M. L., Gossan1, S. E., Gosselin34, M., Gouaty7, R., Graef36, C., Graff63, P. B., Granata66, M., Grant36, A., Gras10, S., Gray37, C., Greco57, G., Green45, A. C., Groot52, P., Grote8, H., Grunewald29, S., Guidi57, G. M., Guo70, X., Gupta14, A., Gupta95, M. K., Gushwa1, K. E., Gustafson1, E. K., Gustafson98, R., Hacker22, J. J., Hall56, B. R., Hall1, E. D., Hammond36, G., Haney99, M., Hanke8, M. M., Hanks37, J., Hanna72, C., Hannam91, M. D., Hanson6, J., Hardwick2, T., Haris106, K., Harms57, J., Harry100, G. M., Harry29, I. W., Hart36, M. J., Hartman5, M. T., Haster45, C. J., Haughian36, K., Heidmann60, A., Heintze5, M. C., Heitmann53, H., Hello23, P., Hemming34, G., Hendry36, M., Heng36, I. S., Hennig36, J., Heptonstall1, A. W., Heurs8, M., Hild36, S., Hoak101, D., Hodge1, K. A., Hofman66, D., Hollitt102, S. E., Holt6, K., Holz75, D. E., Hopkins91, P., Hosken102, D. J., Hough36, J., Houston36, E. A., Howell51, E. J., Hu36, Y. M., Huang73, S., Huerta82, E. A., 103, Huet23, D., Hughey97, B., Husa67, S., Huttner36, S. H., Huynh Dinh6, T., Idrisy72, A., Indik8, N., Ingram37, D. R., Inta71, R., Isa36, H. N., Isac60, J. M., Isi1, M., Islas22, G., Isogai10, T., Iyer15, B. R., Izumi37, K., Jacqmin60, T., Jang77, H., Jani64, K., Jaranowski104, P., Jawahar105, S., Jiménez Forteza67, F., Johnson2, W. W., Jones26, D. I., Jones36, R., Jonker9, R. J. G., Ju51, L., Kalaghatgi24, C. V., Kalogera82, V., Kandhasamy21, S., Kang77, G., Kanner1, J. B., Karki59, S., Kasprzack2, M., 34, 23, Katsavounidis10, E., Katzman6, W., Kaufer17, S., Kaur51, T., Kawabe37, K., Kawazoe8, F., Kéfélian53, F., Kehl69, M. S., Keitel8, D., Kelley35, D. B., Kells1, W., Kennedy86, R., Key85, J. S., Khalaidovski8, A., Khalili49, F. Y., Khan12, I., Khan91, S., Khan95, Z., Khazanov107, E. A., Kijbunchoo37, N., Kim77, C., Kim108, J., Kim109, K., Kim77, N., Kim41, N., Kim108, Y. M., King102, E. J., King37, P. J., Kinzel6, D. L., Kissel37, J. S., Kleybolte27, L., Klimenko5, S., Koehlenbeck8, S. M., Kokeyama2, K., Koley9, S., Kondrashov1, V., Kontos10, A., Korobko27, M., Korth1, W. Z., Kowalska61, I., Kozak1, D. B., Kringel8, V., Królak110, A., 111, Krueger17, C., Kuehn8, G., Kumar69, P., Kuo73, L., Kutynia110, A., Lackey35, B. D., Landry37, M., Lange112, J., Lantz41, B., Lasky113, P. D., Lazzarini1, A., Lazzaro43, C., Leaci28, P., 79, 29, Leavey36, S., Lebigot30, E. O., Lee108, C. H., Lee109, H. K., Lee114, H. M., Lee36, K., Lenon35, A., Leonardi89, M., Leong8, J. R., Leroy23, N., Letendre7, N., Levin113, Y., Levine37, B. M., Li1, T. G. F., Libson10, A., Littenberg115, T. B., Lockerbie105, N. A., Logue36, J., Lombardi101, A. L., Lord35, J. E., Lorenzini12, M., Loriette116, V., Lormand6, M., Losurdo58, G., Lough8, J. D., Lück8, H., Lundgren8, A. P., Luo78, J., Lynch10, R., Ma51, Y., Macdonald41, T., Machenschalk8, B., Macinnis10, M., Macleod2, D. M., Magaña Sandoval35, F., Magee56, R. M., Mageswaran1, M., Majorana28, E., Maksimovic116, I., Malvezzi13, V., Man53, N., Mandel45, I., Mandic83, V., Mangano36, V., Mansell20, G. L., Manske16, M., Mantovani34, M., Marchesoni33, F., 117, Marion7, F., Márka40, S., Márka40, Z., Markosyan41, A. S., Maros1, E., Martelli57, F., Martellini53, L., Martin36, I. W., Martin5, R. M., Martynov1, D. V., Marx1, J. N., Mason10, K., Masserot7, A., Massinger35, T. J., Masso Reid36, M., Matichard10, F., Matone40, L., Mavalvala10, N., Mazumder56, N., Mazzolo8, G., Mccarthy37, R., Mcclelland20, D. E., Mccormick6, S., Mcguire118, S. C., Mcintyre1, G., Mciver1, J., Mcmanus20, D. J., Mcwilliams103, S. T., Meacher72, D., Meadors8, G. D., Meidam9, J., Melatos84, A., Mendell37, G., Mendoza Gandara8, D., Mercer16, R. A., Merilh37, E., Merzougui53, M., Meshkov1, S., Messenger36, C., Messick72, C., Meyers83, P. M., Mezzani28, F., Miao45, H., Michel66, C., Middleton45, H., Mikhailov119, E. E., Milano4, L., Miller10, J., Millhouse31, M., Minenkov13, Y., Ming8, J., Mirshekari120, S., Mishra15, C., Mitra14, S., Mitrofanov49, V. P., Mitselmakher5, G., Mittleman10, R., Moggi19, A., Mohan34, M., Mohapatra10, S. R. P., Montani57, M., Moore88, B. C., Moore121, C. J., Moraru37, D., Moreno37, G., Morriss85, S. R., Mossavi8, K., Mours7, B., Mow Lowry45, C. M., Mueller5, C. L., Mueller5, G., Muir91, A. W., Mukherjee15, A., Mukherjee16, D., Mukherjee85, S., Mukund14, N., Mullavey6, A., Munch102, J., Murphy40, D. J., Murray36, P. G., Mytidis5, A., Nardecchia13, I., Naticchioni28, L., Nayak122, R. K., Necula5, V., Nedkova101, K., Nelemans9, G., Neri46, M., Neunzert98, A., Newton36, G., Nguyen20, T. T., Nielsen8, A. B., Nissanke9, S., Nitz8, A., Nocera34, F., Nolting6, D., Normandin85, M. E. N., Nuttall35, L. K., Oberling37, J., Ochsner16, E., O'Dell123, J., Oelker10, E., Ogin124, G. H., Oh125, J. J., Oh125, S. H., Ohme91, F., Oliver67, M., Oppermann8, P., Oram6, R. J., O'Reilly6, B., O'Shaughnessy112, R., Ottaway102, D. J., Ottens5, R. S., Overmier6, H., Owen71, B. J., Pai106, A., Pai48, S. A., Palamos59, J. R., Palashov107, O., Palliyaguru71, N., Palomba28, C., Pal Singh27, A., Pan73, H., Pankow82, C., Pannarale91, F., Pant48, B. C., Paoletti19, F., Paoli34, A., Papa8, M. A., 29, 16, Paris41, H. R., Parker6, W., Pascucci36, D., Pasqualetti34, A., Passaquieti18, R., Passuello19, D., Patricelli18, B., Patrick41, Z., Pearlstone36, B. L., Pedraza1, M., Pedurand66, R., Pekowsky35, L., Pele6, A., Penn126, S., Perreca1, A., Phelps36, M., Piccinni28, O., Pichot53, M., Piergiovanni57, F., Pierro87, V., Pillant34, G., Pinard66, L., Pinto87, I. M., Pitkin36, M., Poggiani18, R., Popolizio34, P., Post8, A., Powell36, J., Prasad14, J., Predoi91, V., Premachandra113, S. S., Prestegard83, T., Price1, L. R., Prijatelj34, M., Principe87, M., Privitera29, S., Prodi89, G. A., Prokhorov49, L., Puncken8, O., Punturo33, M., Puppo28, P., Pürrer29, M., Qi16, H., Qin51, J., Quetschke85, V., Quintero1, E. A., Quitzow James59, R., Raab37, F. J., Rabeling20, D. S., Radkins37, H., Raffai54, P., Raja48, S., Rakhmanov85, M., Rapagnani28, P., Raymond29, V., Razzano18, M., Re25, V., Read22, J., Reed37, C. M., Regimbau53, T., Rei47, L., Reid50, S., Reitze1, D. H., 5, Rew119, H., Reyes35, S. D., Ricci28, F., Riles98, K., Robertson1, N. A., Robie36, R., Robinet23, F., Rocchi13, A., Rolland7, L., Rollins1, J. G., Roma59, V. J., Romano3, R., Romanov119, G., Romie6, J. H., Rosińska44, D., 127, Rowan36, S., Rüdiger8, A., Ruggi34, P., Ryan37, K., Sachdev1, S., Sadecki37, T., Sadeghian16, L., Salconi34, L., Saleem106, M., Salemi8, F., Samajdar122, A., Sammut84, L., 113, Sanchez1, E. J., Sandberg37, V., Sandeen82, B., Sanders35, J. R., Sassolas66, B., Sathyaprakash91, B. S., Saulson35, P. R., Sauter98, O., Savage37, R. L., Sawadsky17, A., Schale59, P., Schilling8, R., Schmidt8, J., Schmidt1, P., Schnabel27, R., Schofield59, R. M. S., Schönbeck27, A., Schreiber8, E., Schuette8, D., Schutz29, B. F., Scott36, J., Scott20, S. M., Sellers6, D., Sentenac34, D., Sequino13, V., Sergeev107, A., Serna22, G., Setyawati9, Y., Sevigny37, A., Shaddock20, D. A., Shah9, S., Shahriar82, M. S., Shaltev8, M., Shao1, Z., Shapiro41, B., Shawhan63, P., Sheperd16, A., Shoemaker10, D. H., Shoemaker64, D. M., Siellez53, K., Siemens16, X., Sigg37, D., Silva11, A. D., Simakov8, D., Singer1, A., Singh8, A., Singh2, R., Singhal12, A., Sintes67, A. M., Slagmolen20, B. J. J., Smith22, J. R., Smith1, N. D., Smith1, R. J. E., Son125, E. J., Sorazu36, B., Sorrentino47, F., Souradeep14, T., Srivastava95, A. K., Staley40, A., Steinke8, M., Steinlechner36, J., Steinlechner36, S., Steinmeyer8, D., Stephens16, B. C., Stone85, R., Strain36, K. A., Straniero66, N., Stratta57, G., Strauss78, N. A., Strigin49, S., Sturani120, R., Stuver6, A. L., Summerscales128, T. Z., Sun84, L., Sutton91, P. J., Swinkels34, B. L., Szczepańczyk97, M. J., Tacca30, M., Talukder59, D., Tanner5, D. B., Tápai96, M., Tarabrin8, S. P., Taracchini29, A., Taylor1, R., Theeg8, T., Thirugnanasambandam1, M. P., Thomas45, E. G., Thomas6, M., Thomas37, P., Thorne6, K. A., Thorne76, K. S., Thrane113, E., Tiwari12, S., Tiwari91, V., Tokmakov105, K. V., Tomlinson86, C., Tonelli18, M., Torres85, C. V., Torrie1, C. I., Töyrä45, D., Travasso32, F., Traylor6, G., Trifirò21, D., Tringali89, M. C., Trozzo19, L., 129, Tse10, M., Turconi53, M., Tuyenbayev85, D., Ugolini130, D., Unnikrishnan99, C. S., Urban16, A. L., Usman35, S. A., Vahlbruch17, H., Vajente1, G., Valdes85, G., van Bakel9, N., van Beuzekom9, M., van den Brand9, J. F. J., Van Den Broeck9, C., Vander Hyde22, D. C., van der Schaaf9, L., van Heijningen9, J. V., van Veggel36, A. A., Vardaro42, M., Vass1, S., Vasúth38, M., Vaulin10, R., Vecchio45, A., Vedovato43, G., Veitch45, J., Veitch102, P. J., Venkateswara131, K., Verkindt7, D., Vetrano57, F., Viceré57, A., Vinciguerra45, S., Vine50, D. J., Vinet53, J. Y., Vitale10, S., Vo35, T., Vocca32, H., Vorvick37, C., Voss5, D., Vousden45, W. D., Vyatchanin49, S. P., Wade20, A. R., Wade132, L. E., Wade132, M., Walker2, M., Wallace1, L., Walsh8, S., Wang12, G., Wang45, H., Wang45, M., Wang70, X., Wang51, Y., Ward20, R. L., Warner37, J., Was7, M., Weaver37, B., Wei53, L. W., Weinert8, M., Weinstein1, A. J., Weiss10, R., Welborn6, T., Wen51, L., Weßels8, P., Westphal8, T., Wette8, K., Whelan8, J. T., 112, White86, D. J., Whiting5, B. F., Williams1, R. D., Williamson91, A. R., Willis133, J. L., Willke8, B., Wimmer8, M. H., Winkler8, W., Wipf1, C. C., Wittel8, H., Woan36, G., Worden37, J., Wright36, J. L., Wu6, G., Yablon82, J., Yam10, W., Yamamoto1, H., Yancey63, C. C., Yap20, M. J., Yu10, H., Yvert7, M., Zadrożny110, A., Zangrando43, L., Zanolin97, M., Zendri43, J. P., Zevin82, M., Zhang10, F., Zhang1, L., Zhang119, M., Zhang112, Y., Zhao51, C., Zhou82, M., Zhou82, Z., Zhu51, X. J., Zucker1, M. E., Zuraw101, S. E., Zweizig1, J., Allison134, J., 135, Bannister134, K., Bell134, M. E., Chatterjee136, S., Chippendale134, A. P., Edwards134, P. G., Harvey Smith134, L., Ian, Heywood134, 137, Hotan138, A., Indermuehle134, B., Marvil134, J., Mcconnell134, D., Murphy135, T., 139, Popping135, A., 140, Reynolds134, J., Sault84, R. J., 134, Voronkov134, M. A., Whiting134 (The Australian Square Kilometer Array Pathfinder, M. T., Castro Tirado141, A. J., 142, Cunniffe141, R., Jelínek143, M., Tello141, J. C., Oates141, S. R., Hu141, Y. D., Kubánek144, P., Guziy145, S., Castellón146, A., García Cerezo142, A., Muñoz142, V. F., Pérez del Pulgar142, C., Castillo Carrión147, S., Castro Cerón148, J. M., Hudec143, R., 149, Caballero García150, M. D., Páta149, P., Vitek149, S., Adame151, J. A., Konig151, S., Rendón141, F., 151, Mateo Sanguino152, T. de J., Fernández Muñoz153, R., Yock154, P. C., Rattenbury154, N., Allen155, W. H., Querel156, R., Jeong141, S., 157, Park157, I. H., Bai158, J., Cui159, C. h., Fan158, Y., Wang158, C. h., Hiriart160, D., Lee161, W. H., Claret141, A., Sánchez Ramírez141, R., Pandey162, S. B., Mediavilla163, T., Sabau Graziati164, L., Abbott165, T. M. C., Abdalla137, F. B., 166, Allam167, S., Annis167, J., Armstrong168, R., Benoit Lévy166, A., 169, 170, Berger171, E., Bernstein172, R. A., Bertin169, E., 170, Brout173, D., Buckley Geer167, E., Burke174, D. L., 175, Capozzi176, D., Carretero177, J., 178, Castander177, F. J., Chornock179, R., Cowperthwaite171, P. S., Crocce177, M., Cunha174, C. E., D'Andrea26, C. B., 176, da Costa180, L. N., Desai181, S., 182, Diehl167, H. T., Dietrich181, J. P., Doctor183, Z., Drlica Wagner167, A., Drout171, M. R., Eifler173, T. F., 184, Estrada167, J., Evrard98, A. E., Fernandez178, E., Finley167, D. A., Flaugher167, B., Foley185, R. J., 186, Fong187, W. F., Fosalba177, P., Fox188, D. B., Frieman167, J., 183, Fryer189, C. L., Gaztanaga177, E., Gerdes190, D. W., Goldstein191, D. A., 192, Gruen174, D., Gruendl185, R. A., 193, Gutierrez167, G., Herner167, K., Honscheid194, K., 195, James165, D. J., Johnson193, M. D., Johnson193, M. W. G., Karliner186, I., Kasen192, D., 196, Kent167, S., Kessler183, R., Kim192, A. G., Kind185, M. C., Kuehn197, K., Kuropatkin167, N., Lahav166, O., Li198, T. S., Lima180, M., 199, Lin167, H., Maia180, M. A. G., Margutti200, R., Marriner167, J., Martini194, P., 201, Matheson202, T., Melchior168, P., Metzger203, B. D., Miller190, C. J., 204, Miquel178, R., 205, Neilsen167, E., Nichol176, R. C., Nord167, B., Nugent192, P., Ogando180, R., Petravick193, D., Plazas184, A. A., Quataert206, E., Roe192, N., Romer207, A. K., Roodman174, A., Rosell180, A. C., Rykoff174, E. S., Sako173, M., Sanchez208, E., Scarpine167, V., Schindler175, R., Schubnell190, M., Scolnic183, D., Sevilla Noarbe185, I., 208, Sheldon209, E., Smith187, N., Smith165, R. C., Soares Santos167, M., Sobreira180, F., Stebbins167, A., Suchyta173, E., Swanson193, M. E. C., Tarle190, G., Thaler186, J., Thomas176, D., Thomas192, R. C., Tucker167, D. L., Vikram210, V., Walker165, A. R., Wechsler41, R. H., 174, 175, Wester167, W., Yanny167, B., Zhang98, Y., Zuntz211, J., Connaughton212, V., Burns213, E., Goldstein214, A., 378, Briggs215, M. S., Zhang216, B. B., 217, Hui214, C. M., Jenke216, P., Wilson Hodge214, C. A., Bhat216, P. N., Bissaldi218, E., Cleveland212, W., Fitzpatrick216, G., Giles219, M. M., Gibby219, M. H., Greiner220, J., von Kienlin220, A., Kippen221, R. M., Mcbreen222, S., Mailyan216, B., Meegan216, C. A., Paciesas212, W. S., Preece215, R. D., Roberts222, O., Sparke223, L., Stanbro213, M., Toelge220, K., Veres216, P., Yu220, H. F., 224, Blackburn171, L., Ackermann225, M., Ajello226, M., Albert227, A., Anderson228, B., 229, Atwood230, W. B., Axelsson231, M., 232, Baldini227, L., 233, Barbiellini234, G., 235, Bastieri236, D., 237, Bellazzini238, R., Bissaldi239, E., Blandford227, R. D., Bloom227, E. D., Bonino, Raffaella, Bottacini227, E., Brandt242, T. J., Bruel243, P., Buson242, S., 244, 245, Caliandro227, G. A., 246, Cameron227, R. A., Caragiulo239, M., 247, Caraveo248, P. A., Cavazzuti249, E., Charles227, E., Chekhtman250, A., Chiang227, J., Chiaro237, G., Ciprini249, S., 251, Cohen Tanugi252, J., Cominsky253, L. R., Costanza239, F., Cuoco240, A., 241, D'Ammando254, F., 255, de Palma239, F., 256, Desiante240, R., 257, Digel227, S. W., Di Lalla238, N., Di Mauro227, M., Di Venere239, L., Domínguez226, A., Drell227, P. S., Dubois227, R., Favuzzi239, C., Ferrara242, E. C., Franckowiak227, A., Fukazawa258, Y., Funk259, S., Fusco239, P., Gargano239, F., Gasparrini249, D., Giglietto239, N., Giommi249, P., Giordano239, F., Giroletti254, M., Glanzman227, T., Godfrey227, G., Gomez Vargas260, G. A., 261, Green242, D., 262, Grenier263, I. A., Grove264, J. E., Guiriec242, S., Hadasch265, D., Harding242, A. K., Hays242, E., Hewitt266, J. W., Hill227, A. B., 267, Horan243, D., Jogler227, T., Jóhannesson268, G., Johnson227, A. S., Kensei258, S., Kocevski242, D., Kuss238, M., La Mura237, G., 265, Larsson229, S., 231, Latronico240, L., Li269, J., Li229, L., Longo234, F., Loparco239, F., Lovellette264, M. N., Lubrano251, P., Magill262, J., Maldera240, S., Manfreda238, A., Marelli248, M., Mayer225, M., Mazziotta239, M. N., Mcenery242, J. E., Meyer228, M., Michelson227, P. F., Mirabal242, N., Mizuno270, T., Moiseev245, A. A., Monzani227, M. E., Moretti271, E., Morselli261, A., Moskalenko227, I. V., Negro240, M., Nuss252, E., Ohsugi270, T., Omodei227, N., Orienti254, M., Orlando227, E., Ormes272, J. F., Paneque227, D., 271, Perkins242, J. S., Pesce Rollins227, M., 238, Piron252, F., Pivato238, G., Porter227, T. A., Racusin242, J. L., Rainò239, S., Rando236, R., Razzaque273, S., Reimer227, A., Reimer227, O., Salvetti248, D., Saz Parkinson230, P. M., 274, 275, Sgrò238, C., Simone239, D., Siskind276, E. J., Spada238, F., Spandre238, G., Spinelli239, P., Suson277, D. J., Tajima227, H., 278, Thayer227, J. B., Thompson242, D. J., Tibaldo279, L., Torres269, D. F., 280, Troja242, E., Uchiyama281, Y., Venters242, T. M., Vianello227, G., Wood264, K. S., Wood227, M., Zhu262, S., Zimmer228, S., Brocato282, E., Cappellaro283, E., Covino284, S., Grado285, A., Nicastro286, L., Palazzi286, E., Pian286, E., 287, Amati286, L., Antonelli282, L. A., 288, Capaccioli289, M., D'Avanzo284, P., D'Elia282, V., Getman285, F., Giuffrida282, G., Iannicola282, G., Limatola285, L., Lisi282, M., Marinoni282, S., Marrese282, P., 283, Melandri284, A., Piranomonte282, S., Possenti290, A., Pulone282, L., Rossi286, A., Stamerra287, A., 291, Stella282, L., Testa282, V., Tomasella283, L., Yang283 (The GRAvitational Wave Inaf TeAm, S., Bazzano292, A., Bozzo293, E., Brandt294, S., Courvoisier293, T. J. L., Ferrigno293, C., Hanlon295, L., Kuulkers296, E., Laurent297, P., Mereghetti298, S., Roques299, J. P., Savchenko300, V., Ubertini292, P., Kasliwal301, M. M., Singer39, L. P., Cao301, Y., Duggan301, G., Kulkarni301, S. R., Bhalerao14, V., Miller184, A. A., 301, 379, Barlow301, T., Bellm301, E., Manulis302, I., Rana14, J., Laher303, R., Masci303, F., Surace303, J., Rebbapragada184, U., Cook301, D., Van Sistine16, A., Sesar304, B., Perley305, D., Ferreti306, R., Prince301, T., Kendrick307, R., Horesh302 (The Intermediate Palomar Transient Factory, A., Hurley308, K., Golenetskii309, S. V., Aptekar309, R. L., Frederiks309, D. D., Svinkin309, D. S., Rau220, A., Zhang220, X., Smith230, D. M., Cline39, T., 380, Krimm245, H., 310, Abe311, F., Doi312, M., Fujisawa313, K., Kawabata314, K. S., Morokuma312, T., Motohara312, K., Tanaka315, M., Ohta316, K., Yanagisawa317, K., Yoshida314, M., Baltay318, C., Rabinowitz318, D., Ellman318, N., Rostami318, S., Bersier319, D. F., Bode319, M. F., Collins319, C. A., Copperwheat319, C. M., Darnley319, M. J., Galloway320, D. K., 321, Gomboc322, A., 323, Kobayashi319, S., Mazzali319, P., Mundell324, C. G., Piascik319, A. S., Don, Pollacco325, Steele319, I. A., Ulaczyk325, K., Broderick326, J. W., Fender327, R. P., Jonker52, P. G., 328, Rowlinson135, A., 326, 329, Stappers211, B. W., Wijers329 (The Low Frequency Array, R. A. M. J., Lipunov330, V., Gorbovskoy330, E., Tyurina330, N., Kornilov330, V., Balanutsa330, P., Kuznetsov330, A., Buckley331, D., Rebolo332, R., Serra Ricart332, M., Israelian332, G., Budnev333, N. M., Gress333, O., Ivanov333, K., Poleshuk333, V., Tlatov334, A., Yurkov335, V., Kawai336, N., Serino337, M., Negoro338, H., Nakahira339, S., Mihara337, T., Tomida340, H., Ueno340, S., Tsunemi341, H., Matsuoka337, M., Croft342, S., 343, Feng344, L., Franzen345, T. M. O., Gaensler135, B. M., 139, 346, Johnston Hollitt347, M., Kaplan16, D. L., Morales131, M. F., Tingay135, S. J., 345, 348, Wayth135, R. B., 345, Williams345 (The Murchison Wide field Array, A., Smartt349, S. J., Chambers350, K. C., Smith349, K. W., Huber350, M. E., Young349, D. R., Wright349, D. E., Schultz350, A., Denneau350, L., Flewelling350, H., Magnier350, E. A., Primak350, N., Rest351, A., Sherstyuk350, A., Stalder350, B., Stubbs352, C. W., Tonry350, J., Waters350, C., Willman350, M., 353, F. Olivares E., 354, Campbell355, H., Kotak349, R., Sollerman306, J., Smith26, M., Dennefeld356, M., Anderson357, J. P., Botticella285, M. T., Chen220, T. W., Valle285, M. D., Elias Rosa283, N., Fraser355, M., Inserra349, C., Kankare349, E., Kupfer301, T., Harmanen358, J., Galbany353, L., 359, Le Guillou360, L., 361, Lyman325, J. D., Maguire349, K., Mitra361, A., Nicholl171, M., Razza353, A., Terreran283, G., 349, Valenti362, S., 363, Gal Yam364, A., Ćwiek110, A., Ćwiok365, M., Mankiewicz366, L., Opiela366, R., Zaremba365, M., Żarnecki365, A. F., Onken20, C. A., Scalzo20, R. A., Schmidt20, B. P., Wolf20, C., Yuan20, F., Evans367, P. A., Kennea72, J. A., Burrows72, D. N., Campana284, S., Cenko39, S. B., 368, Giommi288, P., Marshall39, F. E., Nousek72, J., O'Brien367, P., Osborne367, J. P., Palmer369, D., Perri282, M., Siegel72, M., Tagliaferri284, G., Klotz370, A., Turpin370, D., Laugier53, R., Beroiz85, M., 371, Peñuela85, T., 372, Macri373, L. M., Oelkers373, R. J., Lambas374, D. G., Vrech374, R., Cabral374, J., Colazo374, C., Dominguez374, M., Sanchez374, B., Gurovich374, S., Lares374, M., Marshall373, J. L., Depoy373, D. L., Padilla375, N., Pereyra85, N. A., Benacquista85, M., Tanvir367, N. R., Wiersema367, K., Levan325, A. J., Steeghs325, D., Hjorth305, J., Fynbo305, J. P. U., Malesani305, D., Milvang Jensen305, B., Watson305, D., Irwin355, M., Fernandez355, C. G., Mcmahon355, R. G., Banerji355, M., Gonzalez Solares355, E., Schulze353, S., 375, de Ugarte Postigo305, A., 376, Thoene376, C. C., Cano377, Z., Rosswog306, S., (Astro)-Particles Physics, Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, Enrico, Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavagliá, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. F., Colla, A., Collette, C. G., Cominsky, L., Constancio, M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., Debra, D., Debreczeni, G., Degallaix, J., DE LAURENTIS, Martina, Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., Derosa, R. T., DE ROSA, Rosario, Desalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, Fabio, Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., Macdonald, T., Machenschalk, B., Macinnis, M., Macleod, D. M., Magaña Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcguire, S. C., Mcintyre, G., Mciver, J., Mcmanus, D. J., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, Leopoldo, Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palliyaguru, N., Palomba, C., Pal Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S. S., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Quitzow James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Van Bakel, N., Van Beuzekom, M., 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., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. P., Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Allison, J., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Harvey Smith, L., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., Mcconnell, D., Murphy, T., Popping, A., Reynolds, J., Sault, R. J., Voronkov, M. A., Whiting, M. T., Castro Tirado, A. J., Cunniffe, R., Jelínek, M., Tello, J. C., Oates, S. R., Hu, Y. D., Kubánek, P., Guziy, S., Castellón, A., García Cerezo, A., Muñoz, V. F., Pérez Del Pulgar, C., Castillo Carrión, S., Castro Cerón, J. M., Hudec, R., Caballero García, M. D., Páta, P., Vitek, S., Adame, J. A., Konig, S., Rendón, F., Mateo Sanguino, T. De J., Fernández Muñoz, R., Yock, P. C., Rattenbury, N., Allen, W. H., Querel, R., Jeong, S., Park, I. H., Bai, J., Cui, C. h., Fan, Y., Wang, C. h., Hiriart, D., Lee, W. H., Claret, A., Sánchez Ramírez, R., Pandey, S. B., Mediavilla, T., Sabau Graziati, L., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit Lévy, A., Berger, E., Bernstein, R. A., Bertin, E., Brout, D., Buckley Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Castander, F. J., Chornock, R., Cowperthwaite, P. S., Crocce, M., Cunha, C. E., D'Andrea, C. B., Da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica Wagner, A., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. F., Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Zhang, B. B., Hui, C. M., Jenke, P., Wilson Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., Von Kienlin, A., Kippen, R. M., Mcbreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. F., Blackburn, L., Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D'Ammando, F., De Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., Mcenery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Parkinson, P. M. Saz, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D'Avanzo, P., D'Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. L., Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Sistine, A. Van, Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, Duncan K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., Olivares, E. F., Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. W., Valle, M. D., Elias Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Guillou, L. Le, Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal Yam, A., Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O'Brien, P., Osborne, J. P., Palmer, D., Perri, M., Siegel, M., Tagliaferri, G., Klotz, A., Turpin, D., Laugier, R., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., Depoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., Mcmahon, R. G., Banerji, M., Gonzalez Solares, E., Schulze, S., De Ugarte Postigo, A., Thoene, C. C., Cano, Z., Rosswog, S., Institut Lumière Matière [Villeurbanne] ( ILM ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Leprince-Ringuet ( LLR ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Particules de Montpellier ( LUPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), LIGO, VIRGO, FERMI LAT, PESSTO, Institut Lumière Matière [Villeurbanne] (ILM), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - 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CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), The LIGO Scientific Collaboration, The Virgo Collaboration, The Australian Square Kilometer Array, Pathfinder (ASKAP) Collaboration, The BOOTES Collaboration, The Dark Energy Survey and the Dark Energy Camera GW-EM Collaborations, The Fermi GBM Collaboration, The Fermi LAT Collaboration, The GRAvitational Wave Inaf TeAm (GRAWITA), The Intermediate Palomar Transient Factory (iPTF) Collaboration, The InterPlanetary Network, The J-GEM Collaboration, The La Silla--QUEST Survey, The Liverpool Telescope Collaboration, The Low Frequency Array (LOFAR) Collaboration, The MASTER Collaboration, The MAXI Collaboration, The Murchison Wide-field Array (MWA) Collaboration, The Pan-STARRS Collaboration, The PESSTO Collaboration, The Pi of the Sky Collaboration, The SkyMapper Collaboration, The Swift Collaboration, The TAROT, Zadko, Algerian National Observatory, C2PU Collaboration, The TOROS Collaboration, The VISTA Collaboration, Calloni, E., De Laurentis, M., De Rosa, R., Garufi, F., Milano, L., Longo, Francesco, Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Montpellier 2 - 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F., M. Constancio J. r., Coulon, J. -. P., D’Antonio, S., Eggenstein, H. -. B., Fournier, J. -. D., A., Gatto, Haster, C. -. J., Huynh-Dinh, T., Isac, J. -. M., Jiménez-Forteza, F., Kim, Y. -. M., Magaña-Sandoval, F., Masso-Reid, M., Mendoza-Gandara, D., C., Michel, Mow-Lowry, C. M., O’Dell, J., O’Reilly, B., O’Shaughnessy, R., Pal-Singh, A., Quitzow-James, R., A., Singh, van Bakel, N., van Beuzekom, M., van den Brand, J. F. J., Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vinet, J. -. Y., M., Wade, Wei, L. -. W., Wessels, P., Zendri, J. -. P., the Virgo Collaboration, Harvey-Smith, L., Ian, Heywood, The Australian Square Kilometer Array Pathfinder (ASKAP) Collaboration, Castro-Tirado, A. J., Hu, Y. -. D., García-Cerezo, A., Pérez del Pulgar, C., Castillo-Carrión, S., Caballero-García, M. D., Mateo Sanguino, T. de J., Fernández-Muñoz, R., Sánchez-Ramírez, R., Sabau-Graziati, L., Benoit-Lévy, A., Buckley-Geer, E., D’Andrea, C. B., da Costa, L. 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Subjects
Astronomy, ADVANCED LIGO, 01 natural sciences, General Relativity and Quantum Cosmology, localization, GW150914, localization, EM follow-up, Observatory, Broadband, BURSTS, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, gravitational wave, QC, media_common, QB, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), gravitational waves, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], methods: observational, Astrophysics - High Energy Astrophysical Phenomena, Cosmology and Gravitation, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], gravitational waves – methods: observational, media_common.quotation_subject, gr-qc, Astrophysics::High Energy Astrophysical Phenomena, GW150914, FOS: Physical sciences, ENERGY CAMERA SEARCH, General Relativity and Quantum Cosmology (gr-qc), NEUTRON-STAR MERGERS, Gravitational waves, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Binary black hole, observational, Astronomy and Astrophysics, Space and Planetary Science [gravitational waves, methods], 0103 physical sciences, GW151226, observational [Methods], EM follow-up, STFC, RADIO, 010308 nuclear & particles physics, Gravitational wave, ST/I001123/1, RCUK, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], COUNTERPARTS, Astronomy and Astrophysic, LIGO, Neutron star, Space and Planetary Science, Sky, ST/L000709/1, EMISSION
Abstract

A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams., Comment: For Supplement, see https://arxiv.org/abs/1604.07864

Published
2016
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35. GaLactic and Extragalactic All-sky Murchison Widefield Array survey eXtended (GLEAM-X) I: Survey Description and Initial Data Release.

Author

Hurley-Walker N, Galvin TJ, Duchesne SW, Zhang X, Morgan J, Hancock PJ, An T, Franzen TMO, Heald G, Ross K, Vernstrom T, Anderson GE, Gaensler BM, Johnston-Hollitt M, Kaplan DL, Riseley CJ, Tingay SJ, and Walker M

Abstract

We describe a new low-frequency wideband radio survey of the southern sky. Observations covering 72-231MHz and Declinations south of +30° have been performed with the Murchison Widefield Array "extended" Phase I I configuration over 2018-2020 and will be processed to form data products including continuum and polarisation images and mosaics, multi-frequency catalogues, transient search data, and ionospheric measurements. From a pilot field described in this work, we publish an initial data release covering 1,447 deg 2 over 4 h≤ RA≤ 13 h, -32.7° ≤ Dec ≤ -20.7°. We process twenty frequency bands sampling 72-231 MHz, with a resolution of 2'-45″, and produce a wideband source-finding image across 170-231MHz with a root-mean-square noise of 1.27 ± 0.15 mJy beam -1 . Source-finding yields 79,124 components, of which 71,320 are fitted spectrally. The catalogue has a completeness of 98% at ~ 50 mJy, and a reliability of 98.2% at 5 σ rising to 99.7% at 7 σ . A catalogue is available from Vizier; images are made available on the GLEAM-X VO server and SkyView. This is the first in a series of data releases from the GLEAM-X survey.

Published
2015
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