Search

Your search keyword '"Farrell, T.J."' showing total 13 results
Start Over Author "Farrell, T.J."
13 results on '"Farrell, T.J."'

5. Characterization of Fluorescence Lifetime of Photofrin and Delta-Aminolevulinic Acid Induced Protoporphyrin IX in Living Cells Using Single- and Two-Photon Excitation.

Author

Russell, J.A., Diamond, K.R., Collins, T.J., Tiedje, H.F., Hayward, J.E., Farrell, T.J., Patterson, M.S., and Qiyin Fang

Abstract

Photodynamic therapy (PDT) is an effective treatment option for various types of invasive tumors. The efficacy of PDT treatment depends strongly on selective cell uptake and selective excitation of the tumor. The characterization of fluorescence lifetimes of photosensitizers localized inside living cells may provide the basis for further investigation of in vivo PDT dosage measurements using time-domain spectroscopy and imaging. In this communication, we investigated the fluorescence lifetime of localized Photofrin and delta-aminolevulinic acid (ALA) induced protoporphyrin IX (PpIX) in living MAT-LyLu (MLL) rat prostate adenocarcinoma cells. The MLL cells were incubated with the photosensitizers, and then treated with light under well-oxygenated conditions using a two-photon fluorescence lifetime imaging microscope (FLIM). Fluorescence lifetime images of these cells were recorded with average lifetimes of 5.5 plusmn 1.2 ns for Photofrin and 6.3 plusmn 1.2 ns for ALA-induced PpIX. When localized in cells, the lifetimes of both photosensitizers were found to be significantly shorter than those measured in organic solutions. The result for PpIX is consistent with literature values, while the lifetime of Photofrin is shorter than what has been reported. These results suggest that time-domain methods measuring photosensitizer lifetime changes may be good candidates for in vivo PDT dosage monitoring. [ABSTRACT FROM PUBLISHER]

Published
2008
Full Text
View/download PDF

6. The Anglo-Australian Observatory 2dF facility.

Author

Lewis, I.J., Cannon, R.D., Taylor, K., Glazebrook, K., Bailey, J.A., Baldry, I.K., Barton, J.R., Bridges, T.J., Dalton, G.B., Farrell, T.J., Gray, P.M., Lankshear, A., McCowage, C., Parry, I.R., Sharples, R.M., Shortridge, K., Smith, G.A., Stevenson, J., Straede, J.O., and Waller, L.G.

Subjects
TELESCOPE maintenance & repair, SPECTRUM analysis
Abstract

The 2dF (Two-degree Field) facility at the prime focus of the Anglo-Australian Telescope provides multiple-object spectroscopy over a 2° field of view. Up to 400 target fibres can be independently positioned by a complex robot. Two spectrographs provide spectra with resolutions of between 500 and 2000, over wavelength ranges of 440 and 110 nm respectively. The 2dF facility began routine observations in 1997. 2dF was designed primarily for galaxy redshift surveys and has a number of innovative features. The large corrector lens incorporates an atmospheric dispersion compensator, essential for wide wavelength coverage with small-diameter fibres. The instrument has two full sets of fibres on separate field plates, so that re-configuring can be done in parallel with observing. The robot positioner places one fibre every 6 s, to a precision of 0.3 arcsec (20 μm) over the full field. All components of 2dF, including the spectrographs, are mounted on a 5-m diameter telescope top end ring for ease of handling and to keep the optical fibres short in order to maximize UV throughput. There is a pipeline data reduction system which allows each data set to be fully analysed while the next field is being observed. 2dF has achieved its initial astronomical goals. The redshift surveys obtain spectra at the rate of 2500 galaxies per night, yielding a total of about 200 000 objects in the first four years. Typically a B=19 galaxy gives a spectrum with a signal-to-noise ratio of better than 10 per pixel in less than an hour; redshifts are derived for about 95 per cent of all galaxies, with 99 per cent reliability or better. Total system throughput is about 5 per cent. The failure rate of the positioner and fibre system is about 1:10 000 moves or once every few nights, and recovery time is usually short. In this paper we provide the historical background to the 2dF facility, the design philosophy, a full technical description and a summary of the performance of the instrument. We also briefly review its scientific applications and possible future developments. [ABSTRACT FROM AUTHOR]

Published
2002
Full Text
View/download PDF

7. Follow up of GW170817 and its electromagnetic counterpart by Australian-led observing programmes

Author

Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J.R., Anderson, G.E., Ashley, M.C.B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M.S., Bian, F., Bland, P.A., Boer, M., Booler, T., Brandeker, A., Brown, I.S., Buckley, D.A.H., Chang, S.-W., Coward, D.M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupák, M., de Gois, J.S., Deller, A., Devillepoix, H.A.R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T.J., Franzen, T., Gaensler, B.M., Galloway, D.K., Gendre, B., Giblin, T., Goobar, A., Green, J., Hancock, P.J., Hartig, B.A.D., Howell, E.J., Horsley, L., Hotan, A., Howie, R.M., Hu, L., Hu, Y., James, C.W., Johnston, S., Johnston-Hollitt, M., Kaplan, D.L., Kasliwal, M., Keane, E.F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L.C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D.E., McCully, C., Möller, A., Morales, M.F., Morris, D., Murphy, T., Noysena, K., Onken, C.A., Orange, N.B., Osłowski, S., Pallot, D., Paxman, J., Potter, S.B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E.M., Sansom, E.K., Scalzo, R.A., Schmidt, B.P., Scott, S.M., Seghouani, N., Shang, Z., Shannon, R.M., Shao, L., Shara, M.M., Sharp, R., Sokolowski, M., Sollerman, J., Staff, J., Steele, K., Sun, T., Suntzeff, N.B., Tao, C., Tingay, S., Towner, M.C., Thierry, P., Trott, C., Tucker, B.E., Väisänen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., Zovaro, H., Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J.R., Anderson, G.E., Ashley, M.C.B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M.S., Bian, F., Bland, P.A., Boer, M., Booler, T., Brandeker, A., Brown, I.S., Buckley, D.A.H., Chang, S.-W., Coward, D.M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupák, M., de Gois, J.S., Deller, A., Devillepoix, H.A.R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T.J., Franzen, T., Gaensler, B.M., Galloway, D.K., Gendre, B., Giblin, T., Goobar, A., Green, J., Hancock, P.J., Hartig, B.A.D., Howell, E.J., Horsley, L., Hotan, A., Howie, R.M., Hu, L., Hu, Y., James, C.W., Johnston, S., Johnston-Hollitt, M., Kaplan, D.L., Kasliwal, M., Keane, E.F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L.C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D.E., McCully, C., Möller, A., Morales, M.F., Morris, D., Murphy, T., Noysena, K., Onken, C.A., Orange, N.B., Osłowski, S., Pallot, D., Paxman, J., Potter, S.B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E.M., Sansom, E.K., Scalzo, R.A., Schmidt, B.P., Scott, S.M., Seghouani, N., Shang, Z., Shannon, R.M., Shao, L., Shara, M.M., Sharp, R., Sokolowski, M., Sollerman, J., Staff, J., Steele, K., Sun, T., Suntzeff, N.B., Tao, C., Tingay, S., Towner, M.C., Thierry, P., Trott, C., Tucker, B.E., Väisänen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., and Zovaro, H.

Abstract

The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early- to late-time multi-wavelength observations, including optical imaging and spectroscopy, mid-infrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source emission cooled from approximately 6 400 K to 2 100 K over a 7-d period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (~2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor.

Full Text
View/download PDF

8. Follow up of GW170817 and its electromagnetic counterpart by Australian-led observing programmes

Author

Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J.R., Anderson, G.E., Ashley, M.C.B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M.S., Bian, F., Bland, P.A., Boer, M., Booler, T., Brandeker, A., Brown, I.S., Buckley, D.A.H., Chang, S.-W., Coward, D.M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupák, M., de Gois, J.S., Deller, A., Devillepoix, H.A.R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T.J., Franzen, T., Gaensler, B.M., Galloway, D.K., Gendre, B., Giblin, T., Goobar, A., Green, J., Hancock, P.J., Hartig, B.A.D., Howell, E.J., Horsley, L., Hotan, A., Howie, R.M., Hu, L., Hu, Y., James, C.W., Johnston, S., Johnston-Hollitt, M., Kaplan, D.L., Kasliwal, M., Keane, E.F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L.C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D.E., McCully, C., Möller, A., Morales, M.F., Morris, D., Murphy, T., Noysena, K., Onken, C.A., Orange, N.B., Osłowski, S., Pallot, D., Paxman, J., Potter, S.B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E.M., Sansom, E.K., Scalzo, R.A., Schmidt, B.P., Scott, S.M., Seghouani, N., Shang, Z., Shannon, R.M., Shao, L., Shara, M.M., Sharp, R., Sokolowski, M., Sollerman, J., Staff, J., Steele, K., Sun, T., Suntzeff, N.B., Tao, C., Tingay, S., Towner, M.C., Thierry, P., Trott, C., Tucker, B.E., Väisänen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., Zovaro, H., Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J.R., Anderson, G.E., Ashley, M.C.B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M.S., Bian, F., Bland, P.A., Boer, M., Booler, T., Brandeker, A., Brown, I.S., Buckley, D.A.H., Chang, S.-W., Coward, D.M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupák, M., de Gois, J.S., Deller, A., Devillepoix, H.A.R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T.J., Franzen, T., Gaensler, B.M., Galloway, D.K., Gendre, B., Giblin, T., Goobar, A., Green, J., Hancock, P.J., Hartig, B.A.D., Howell, E.J., Horsley, L., Hotan, A., Howie, R.M., Hu, L., Hu, Y., James, C.W., Johnston, S., Johnston-Hollitt, M., Kaplan, D.L., Kasliwal, M., Keane, E.F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L.C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D.E., McCully, C., Möller, A., Morales, M.F., Morris, D., Murphy, T., Noysena, K., Onken, C.A., Orange, N.B., Osłowski, S., Pallot, D., Paxman, J., Potter, S.B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E.M., Sansom, E.K., Scalzo, R.A., Schmidt, B.P., Scott, S.M., Seghouani, N., Shang, Z., Shannon, R.M., Shao, L., Shara, M.M., Sharp, R., Sokolowski, M., Sollerman, J., Staff, J., Steele, K., Sun, T., Suntzeff, N.B., Tao, C., Tingay, S., Towner, M.C., Thierry, P., Trott, C., Tucker, B.E., Väisänen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., and Zovaro, H.

Abstract

The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early- to late-time multi-wavelength observations, including optical imaging and spectroscopy, mid-infrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source emission cooled from approximately 6 400 K to 2 100 K over a 7-d period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (~2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor.

Full Text
View/download PDF

9. Follow up of GW170817 and its electromagnetic counterpart by Australian-led observing programmes

Author

Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J.R., Anderson, G.E., Ashley, M.C.B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M.S., Bian, F., Bland, P.A., Boer, M., Booler, T., Brandeker, A., Brown, I.S., Buckley, D.A.H., Chang, S.-W., Coward, D.M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupák, M., de Gois, J.S., Deller, A., Devillepoix, H.A.R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T.J., Franzen, T., Gaensler, B.M., Galloway, D.K., Gendre, B., Giblin, T., Goobar, A., Green, J., Hancock, P.J., Hartig, B.A.D., Howell, E.J., Horsley, L., Hotan, A., Howie, R.M., Hu, L., Hu, Y., James, C.W., Johnston, S., Johnston-Hollitt, M., Kaplan, D.L., Kasliwal, M., Keane, E.F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L.C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D.E., McCully, C., Möller, A., Morales, M.F., Morris, D., Murphy, T., Noysena, K., Onken, C.A., Orange, N.B., Osłowski, S., Pallot, D., Paxman, J., Potter, S.B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E.M., Sansom, E.K., Scalzo, R.A., Schmidt, B.P., Scott, S.M., Seghouani, N., Shang, Z., Shannon, R.M., Shao, L., Shara, M.M., Sharp, R., Sokolowski, M., Sollerman, J., Staff, J., Steele, K., Sun, T., Suntzeff, N.B., Tao, C., Tingay, S., Towner, M.C., Thierry, P., Trott, C., Tucker, B.E., Väisänen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., Zovaro, H., Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J.R., Anderson, G.E., Ashley, M.C.B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M.S., Bian, F., Bland, P.A., Boer, M., Booler, T., Brandeker, A., Brown, I.S., Buckley, D.A.H., Chang, S.-W., Coward, D.M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupák, M., de Gois, J.S., Deller, A., Devillepoix, H.A.R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T.J., Franzen, T., Gaensler, B.M., Galloway, D.K., Gendre, B., Giblin, T., Goobar, A., Green, J., Hancock, P.J., Hartig, B.A.D., Howell, E.J., Horsley, L., Hotan, A., Howie, R.M., Hu, L., Hu, Y., James, C.W., Johnston, S., Johnston-Hollitt, M., Kaplan, D.L., Kasliwal, M., Keane, E.F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L.C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D.E., McCully, C., Möller, A., Morales, M.F., Morris, D., Murphy, T., Noysena, K., Onken, C.A., Orange, N.B., Osłowski, S., Pallot, D., Paxman, J., Potter, S.B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E.M., Sansom, E.K., Scalzo, R.A., Schmidt, B.P., Scott, S.M., Seghouani, N., Shang, Z., Shannon, R.M., Shao, L., Shara, M.M., Sharp, R., Sokolowski, M., Sollerman, J., Staff, J., Steele, K., Sun, T., Suntzeff, N.B., Tao, C., Tingay, S., Towner, M.C., Thierry, P., Trott, C., Tucker, B.E., Väisänen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., and Zovaro, H.

Abstract

The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early- to late-time multi-wavelength observations, including optical imaging and spectroscopy, mid-infrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source emission cooled from approximately 6 400 K to 2 100 K over a 7-d period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (~2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor.

Full Text
View/download PDF

10. Follow up of GW170817 and its electromagnetic counterpart by Australian-led observing programmes

Author

Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J.R., Anderson, G.E., Ashley, M.C.B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M.S., Bian, F., Bland, P.A., Boer, M., Booler, T., Brandeker, A., Brown, I.S., Buckley, D.A.H., Chang, S.-W., Coward, D.M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupák, M., de Gois, J.S., Deller, A., Devillepoix, H.A.R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T.J., Franzen, T., Gaensler, B.M., Galloway, D.K., Gendre, B., Giblin, T., Goobar, A., Green, J., Hancock, P.J., Hartig, B.A.D., Howell, E.J., Horsley, L., Hotan, A., Howie, R.M., Hu, L., Hu, Y., James, C.W., Johnston, S., Johnston-Hollitt, M., Kaplan, D.L., Kasliwal, M., Keane, E.F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L.C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D.E., McCully, C., Möller, A., Morales, M.F., Morris, D., Murphy, T., Noysena, K., Onken, C.A., Orange, N.B., Osłowski, S., Pallot, D., Paxman, J., Potter, S.B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E.M., Sansom, E.K., Scalzo, R.A., Schmidt, B.P., Scott, S.M., Seghouani, N., Shang, Z., Shannon, R.M., Shao, L., Shara, M.M., Sharp, R., Sokolowski, M., Sollerman, J., Staff, J., Steele, K., Sun, T., Suntzeff, N.B., Tao, C., Tingay, S., Towner, M.C., Thierry, P., Trott, C., Tucker, B.E., Väisänen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., Zovaro, H., Andreoni, I., Ackley, K., Cooke, J., Acharyya, A., Allison, J.R., Anderson, G.E., Ashley, M.C.B., Baade, D., Bailes, M., Bannister, K., Beardsley, A., Bessell, M.S., Bian, F., Bland, P.A., Boer, M., Booler, T., Brandeker, A., Brown, I.S., Buckley, D.A.H., Chang, S.-W., Coward, D.M., Crawford, S., Crisp, H., Crosse, B., Cucchiara, A., Cupák, M., de Gois, J.S., Deller, A., Devillepoix, H.A.R., Dobie, D., Elmer, E., Emrich, D., Farah, W., Farrell, T.J., Franzen, T., Gaensler, B.M., Galloway, D.K., Gendre, B., Giblin, T., Goobar, A., Green, J., Hancock, P.J., Hartig, B.A.D., Howell, E.J., Horsley, L., Hotan, A., Howie, R.M., Hu, L., Hu, Y., James, C.W., Johnston, S., Johnston-Hollitt, M., Kaplan, D.L., Kasliwal, M., Keane, E.F., Kenney, D., Klotz, A., Lau, R., Laugier, R., Lenc, E., Li, X., Liang, E., Lidman, C., Luvaul, L.C., Lynch, C., Ma, B., Macpherson, D., Mao, J., McClelland, D.E., McCully, C., Möller, A., Morales, M.F., Morris, D., Murphy, T., Noysena, K., Onken, C.A., Orange, N.B., Osłowski, S., Pallot, D., Paxman, J., Potter, S.B., Pritchard, T., Raja, W., Ridden-Harper, R., Romero-Colmenero, E., Sadler, E.M., Sansom, E.K., Scalzo, R.A., Schmidt, B.P., Scott, S.M., Seghouani, N., Shang, Z., Shannon, R.M., Shao, L., Shara, M.M., Sharp, R., Sokolowski, M., Sollerman, J., Staff, J., Steele, K., Sun, T., Suntzeff, N.B., Tao, C., Tingay, S., Towner, M.C., Thierry, P., Trott, C., Tucker, B.E., Väisänen, P., Krishnan, V. Venkatraman, Walker, M., Wang, L., Wang, X., Wayth, R., Whiting, M., Williams, A., Williams, T., Wolf, C., Wu, C., Wu, X., Yang, J., Yuan, X., Zhang, H., Zhou, J., and Zovaro, H.

Abstract

The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early- to late-time multi-wavelength observations, including optical imaging and spectroscopy, mid-infrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source emission cooled from approximately 6 400 K to 2 100 K over a 7-d period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (~2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor.

Full Text
View/download PDF

11. Behavioural family counselling reduces drug use in opioid-dependent men.

Author

Fals-Stewart, W. and Farrell, T.J.

Subjects
*DRUG abuse treatment, *OPIOID abuse, *BEHAVIOR therapy, *NALTREXONE, *FAMILY counseling, *OPIUM abuse, *PSYCHOTHERAPY, *THERAPEUTICS
Abstract

Compares the effectiveness of behavioral family counseling and taking naltrexone in the presence of a family member than individual-based treatment without family involvement. Prescription of naltrexone to the participants; Main outcome measures including abstinence from opioids assessed by Time Line Follow Back interview; Results showing that abstinence from opioids was greater in the behavior family counseling group than in the individual treatment group during treatment and at 12 months follow up; Conclusion that behavior family treatment improves outcomes better than individual treatment in men with opioid dependence.

Published
2003

Catalog

Books, media, physical & digital resources
See catalog results