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7 results on '"Sansom, E.K."'

1. A Global Fireball Observatory

Author

Devillepoix, H.A.R., Cupák, M., Bland, P.A., Sansom, E.K., Towner, M.C., Howie, R.M., Hartig, B.A.D., Jansen-Sturgeon, T., Shober, P.M., Anderson, S.L., Benedix, G.K., Busan, D., Sayers, R., Jenniskens, P., Albers, J., Herd, C.D.K., Hill, P.J.A., Brown, P.G., Krzeminski, Z., Osinski, G.R., Aoudjehane, H. Chennaoui, Benkhaldoun, Z., Jabiri, A., Guennoun, M., Barka, A., Darhmaoui, H., Daly, L., Collins, G.S., McMullan, S., Suttle, M.D., Ireland, T., Bonning, G., Baeza, L., Alrefay, T.Y., Horner, J., Swindle, T.D., Hergenrother, C.W., Fries, M.D., Tomkins, A., Langendam, A., Rushmer, T., O’Neill, C., Janches, D., Hormaechea, J.L., Shaw, C., Young, J.S., Alexander, M., Mardon, A.D., and Tate, J.R.

Published
2020
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2. Mineralogy, petrology, geochemistry, and chronology of the Murrili (H5) meteorite fall: The third recovered fall from the Desert Fireball Network

Author

Anderson, S., Benedix, G.K., Forman, L.V., Daly, Luke, Greenwood, R.C., Franchi, I.A., Friedrich, J.M., Macke, R., Wiggins, S., Britt, D., Cadogan, J.M., Meier, M.M.M., Maden, C., Busemann, H., Welten, K.C., Caffee, M.W., Jourdan, F., Mayers, C., Kennedy, T., Godel, B., Esteban, L., Merigot, K., Bevan, A.W.R., Bland, P.A., Paxman, J., Towner, M.C., Cupak, M., Sansom, E.K., Howie, R., Devillepoix, H., Jansen‐Sturgeon, T., Stuart, D., and Strangway, D.

Abstract

Murrili, the third meteorite recovered by the Desert Fireball Network, is analyzed using mineralogy, oxygen isotopes, bulk chemistry, physical properties, noble gases, and cosmogenic radionuclides. The modal mineralogy, bulk chemistry, magnetic susceptibility, physical properties, and oxygen isotopes of Murrili point to it being an H5 ordinary chondrite. It is heterogeneously shocked (S2–S5), depending on the method used to determine it, although Murrili is not obviously brecciated in texture. Cosmogenic radionuclides yield a cosmic ray exposure age of 6–8 Ma, and a pre‐atmospheric meteoroid size of 15–20 cm in radius. Murrili’s fall and subsequent month‐long embedment into the salt lake Kati Thanda significantly altered the whole rock, evident in its Mössbauer spectra, and visual inspection of cut sections. Murrili may have experienced minor, but subsequent, impacts after its formation 4475.3 ± 2.3 Ma, which left it heterogeneously shocked.

Published
2021

3. Recreating the OSIRIS-REx slingshot manoeuvre from a network of ground-based sensors

Author

Jansen-Sturgeon, T, Hartig, B.A.D., Madsen, Gregory J., Bland, Philip, Sansom, E.K., Devillepoix, Hadrien, Howie, R.M., Cupak, M, Towner, M.C., Cox, Morgan A., Nevill, Nicole D., Hoskins, Zacchary N. P., Bonning, Geoffrey, Calcino, Josh, Clark, Jake T., Henson, Bryce, Langendam, Andrew, Matthews, Samuel J., McClafferty, Terence P., Mitchell, Jennifer T., O'Neill, Craig, Smith, Luke T., Tait, Alastair, Jansen-Sturgeon, T, Hartig, B.A.D., Madsen, Gregory J., Bland, Philip, Sansom, E.K., Devillepoix, Hadrien, Howie, R.M., Cupak, M, Towner, M.C., Cox, Morgan A., Nevill, Nicole D., Hoskins, Zacchary N. P., Bonning, Geoffrey, Calcino, Josh, Clark, Jake T., Henson, Bryce, Langendam, Andrew, Matthews, Samuel J., McClafferty, Terence P., Mitchell, Jennifer T., O'Neill, Craig, Smith, Luke T., and Tait, Alastair

Abstract

Optical tracking systems typically trade off between astrometric precision and field of view. In this work, we showcase a networked approach to optical tracking using very wide field-of-view imagers that have relatively low astrometric precision on the scheduled OSIRIS-REx slingshot manoeuvre around Earth on 22 Sep 2017. As part of a trajectory designed to get OSIRIS-REx to NEO 101955 Bennu, this flyby event was viewed from 13 remote sensors spread across Australia and New Zealand to promote triangulatable observations. Each observatory in this portable network was constructed to be as lightweight and portable as possible, with hardware based off the successful design of the Desert Fireball Network. Over a 4-h collection window, we gathered 15 439 images of the night sky in the predicted direction of the OSIRIS-REx spacecraft. Using a specially developed streak detection and orbit determination data pipeline, we detected 2 090 line-of-sight observations. Our fitted orbit was determined to be within about 10 km of orbital telemetry along the observed 109 262 km length of OSIRIS-REx trajectory, and thus demonstrating the impressive capability of a networked approach to Space Surveillance and Tracking.

Published
2020

4. 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.

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5. 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
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6. 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
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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.

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