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101. Microlensing Binaries with Candidate Brown Dwarf Companions

Author

Shin, I.-G, Han, C., Gould, A., Udalski, A., Sumi, T., Dominik, M., Beaulieu, J.-P, Tsapras, Y., Bozza, V., Szyman´ski, M. K., Kubiak, M., Soszyn´ski, I., Pietrzyn´ski, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Kobara, S., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Omori, K., Perrott, Y. C., Rattenbury, N., Saito, To, Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Christie, G. W., Depoy, D. L., Dong, S., Gal-Yam, A., Gaudi, B. S., Hung, L.-W, Janczak, J., Kaspi, S., Maoz, D., McCormick, J., McGregor, D., Moorhouse, D., Muñoz, J. A., Natusch, T., Nelson, C., Pogge, R. W., Tan, T.-G, Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Malamud, U., Yee, J. C., Choi, J.-Y, Jung, Y.-K, Park, H., Lee, C.-U, Park, B.-G, Koo, J.-R, Bajek, D., Bramich, D. M., Browne, P., Horne, K., Ipatov, S., Snodgrass, C., Steele, I., Street, R., Alsubai, K. A., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S, Grundahl, F., Gu, C.-H, Hardis, S., Harpsøe, K., Hinse, T. C., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Hornstrup, Allan, Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Zimmer, F., Albrow, M. D., Batista, V., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cassan, A., Cole, A., Cook, K. H., Corrales, E., Coutures, Ch, Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque´, P., Greenhill, J., Hill, K., Hoffman, M., Kane, S. R., Kubas, D., Marquette, J.-B, Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Vinter, C., Zub, M., Shin, I.-G, Han, C., Gould, A., Udalski, A., Sumi, T., Dominik, M., Beaulieu, J.-P, Tsapras, Y., Bozza, V., Szyman´ski, M. K., Kubiak, M., Soszyn´ski, I., Pietrzyn´ski, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Kobara, S., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Omori, K., Perrott, Y. C., Rattenbury, N., Saito, To, Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Christie, G. W., Depoy, D. L., Dong, S., Gal-Yam, A., Gaudi, B. S., Hung, L.-W, Janczak, J., Kaspi, S., Maoz, D., McCormick, J., McGregor, D., Moorhouse, D., Muñoz, J. A., Natusch, T., Nelson, C., Pogge, R. W., Tan, T.-G, Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Malamud, U., Yee, J. C., Choi, J.-Y, Jung, Y.-K, Park, H., Lee, C.-U, Park, B.-G, Koo, J.-R, Bajek, D., Bramich, D. M., Browne, P., Horne, K., Ipatov, S., Snodgrass, C., Steele, I., Street, R., Alsubai, K. A., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S, Grundahl, F., Gu, C.-H, Hardis, S., Harpsøe, K., Hinse, T. C., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Hornstrup, Allan, Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Zimmer, F., Albrow, M. D., Batista, V., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cassan, A., Cole, A., Cook, K. H., Corrales, E., Coutures, Ch, Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque´, P., Greenhill, J., Hill, K., Hoffman, M., Kane, S. R., Kubas, D., Marquette, J.-B, Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Vinter, C., and Zub, M.

Abstract

Brown dwarfs are important objects because they may provide a missing link between stars and planets, two populations that have dramatically different formation histories. In this paper, we present the candidate binaries with brown dwarf companions that are found by analyzing binary microlensing events discovered during the 2004-2011 observation seasons. Based on the low mass ratio criterion of q <0.2, we found seven candidate events: OGLE-2004-BLG-035, OGLE-2004-BLG-039, OGLE-2007-BLG-006, OGLE-2007-BLG-399/MOA-2007-BLG-334, MOA-2011-BLG-104/OGLE-2011-BLG-0172, MOA-2011-BLG-149, and MOA-201-BLG-278/OGLE-2011-BLG-012N. Among them, we are able to confirm that the companions of the lenses of MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149 are brown dwarfs by determining the mass of the lens based on the simultaneous measurement of the Einstein radius and the lens parallax. The measured masses of the brown dwarf companions are 0.02 ± 0.01 M⊙ and 0.019 ± 0.002 M⊙ for MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149, respectively, and both companions are orbiting low-mass M dwarf host stars. More microlensing brown dwarfs are expected to be detected as the number of lensing events with well-covered light curves increases with new-generation searches.

Published
2012

102. A new type of Ambiguity in the Planet and Binary Interpretations of Central Perturbations of High-magnification Gravitational Microlensing Events

Author

Choi, J.-Y, Shin, I.-G, Han, C., Udalski, A., Sumi, T., Gould, A., Bozza, V., Dominik, M., Fouque´, P., Horne, K., Szyman´ski, M. K., Kubiak, M., Soszyn´ski, I., Pietrzyn´ski, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., OGLE Collaboration, Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Kobara, S., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohmori, K., Ohnishi, K., Rattenbury, N. J., Saito, To, Sullivan, D. J., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., MOA Collaboration, Bramich, D. M., Snodgrass, C., Steele, I. A., Street, R. A., Tsapras, Y., RoboNet Collaboration, Alsubai, K. A., Browne, P., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S, Grundahl, F., Gu, C.-H, Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, Allan, Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lunkkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Almeida, L. A., Batista, V., Christie, G., DePoy, D. L., Dong, Subo, Gaudi, B. S., Henderson, C., Jablonski, F., Lee, C.-U, McCormick, J., McGregor, D., Moorhouse, D., Natusch, T., Ngan, H., Pogge, R. W., Tan, T.-G, Thornley, G., Yee, J. C., Albrow, M. D., Bachelet, E., Beaulieu, J.-P, Brillant, S., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Greenhill, J., Kubas, D., Marquette, J.-B, Menzies, J. W., Sahu, K. C., Zub, M., Choi, J.-Y, Shin, I.-G, Han, C., Udalski, A., Sumi, T., Gould, A., Bozza, V., Dominik, M., Fouque´, P., Horne, K., Szyman´ski, M. K., Kubiak, M., Soszyn´ski, I., Pietrzyn´ski, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., OGLE Collaboration, Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Kobara, S., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohmori, K., Ohnishi, K., Rattenbury, N. J., Saito, To, Sullivan, D. J., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., MOA Collaboration, Bramich, D. M., Snodgrass, C., Steele, I. A., Street, R. A., Tsapras, Y., RoboNet Collaboration, Alsubai, K. A., Browne, P., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S, Grundahl, F., Gu, C.-H, Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, Allan, Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lunkkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Almeida, L. A., Batista, V., Christie, G., DePoy, D. L., Dong, Subo, Gaudi, B. S., Henderson, C., Jablonski, F., Lee, C.-U, McCormick, J., McGregor, D., Moorhouse, D., Natusch, T., Ngan, H., Pogge, R. W., Tan, T.-G, Thornley, G., Yee, J. C., Albrow, M. D., Bachelet, E., Beaulieu, J.-P, Brillant, S., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Greenhill, J., Kubas, D., Marquette, J.-B, Menzies, J. W., Sahu, K. C., and Zub, M.

Abstract

High-magnification microlensing events provide an important channel to detect planets. Perturbations near the peak of a high-magnification event can be produced either by a planet or a binary companion. It is known that central perturbations induced by both types of companions can be generally distinguished due to the essentially different magnification pattern around caustics. In this paper, we present a case of central perturbations for which it is difficult to distinguish the planetary and binary interpretations. The peak of a lensing light curve affected by this perturbation appears to be blunt and flat. For a planetary case, this perturbation occurs when the source trajectory passes the negative perturbation region behind the back end of an arrowhead-shaped central caustic. For a binary case, a similar perturbation occurs for a source trajectory passing through the negative perturbation region between two cusps of an astroid-shaped caustic. We demonstrate the degeneracy for two high-magnification events of OGLE-2011-BLG-0526 and OGLE-2011-BLG-0950/MOA-2011-BLG-336. For OGLE-2011-BLG-0526, the χ2 difference between the planetary and binary model is ~3, implying that the degeneracy is very severe. For OGLE-2011-BLG-0950/MOA-2011-BLG-336, the stellar binary model is formally excluded with Δχ2 ~ 105 and the planetary model is preferred. However, it is difficult to claim a planet discovery because systematic residuals of data from the planetary model are larger than the difference between the planetary and binary models. Considering that two events observed during a single season suffer from such a degeneracy, it is expected that central perturbations experiencing this type of degeneracy is common.

Published
2012

103. Characterizing low-mass binaries from observation of long-timescale caustic-crossing gravitational microlensing events

Author

Shin, I.-G, Han, C., Choi, J.-Y, Udalski, A., Sumi, T., Gould, A., Bozza, V., Dominik, M., Fouque´, P., Horne, K., Szyman´ski, M. K., Kubiak, M., Soszyn´ski, I., Pietrzyn´ski, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Kobara, S., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohmori, K., Ohnishi, K., Rattenbury, N. J., Saito, To, Sullivan, D. J., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., MOA Collaboration, Bramich, D. M., Snodgrass, C., Steele, I. A., Street, R. A., Tsapras, Y., RoboNet Collaboration, Alsubai, K. A., Browne, P., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S, Grundahl, Frank, Gu, C.-H, Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Hornstrup, Allan, Hundertmark, M., Jessen-Hansen, Jens, Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lunkkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Almeida, L. A., Batista, V., Christie, G., DePoy, D. L., Dong, Subo, Gaudi, B. S., Henderson, C., Jablonski, F., Lee, C.-U, McCormick, J., McGregor, D., Moorhouse, D., Natusch, T., Ngan, H., Park, S.-Y., Pogge, R. W., Tan, T.-G, Thornley, G., Yee, J. C., Albrow, M. D., Bachelet, E., Beaulieu, J.-P, Brillant, S., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Greenhill, J., Kubas, D., Marquette, J.-B, Menzies, J. W., Sahu, K. C., Zub, M., Shin, I.-G, Han, C., Choi, J.-Y, Udalski, A., Sumi, T., Gould, A., Bozza, V., Dominik, M., Fouque´, P., Horne, K., Szyman´ski, M. K., Kubiak, M., Soszyn´ski, I., Pietrzyn´ski, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Kobara, S., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohmori, K., Ohnishi, K., Rattenbury, N. J., Saito, To, Sullivan, D. J., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., MOA Collaboration, Bramich, D. M., Snodgrass, C., Steele, I. A., Street, R. A., Tsapras, Y., RoboNet Collaboration, Alsubai, K. A., Browne, P., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S, Grundahl, Frank, Gu, C.-H, Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Hornstrup, Allan, Hundertmark, M., Jessen-Hansen, Jens, Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lunkkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Almeida, L. A., Batista, V., Christie, G., DePoy, D. L., Dong, Subo, Gaudi, B. S., Henderson, C., Jablonski, F., Lee, C.-U, McCormick, J., McGregor, D., Moorhouse, D., Natusch, T., Ngan, H., Park, S.-Y., Pogge, R. W., Tan, T.-G, Thornley, G., Yee, J. C., Albrow, M. D., Bachelet, E., Beaulieu, J.-P, Brillant, S., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Greenhill, J., Kubas, D., Marquette, J.-B, Menzies, J. W., Sahu, K. C., and Zub, M.

Abstract

Despite the astrophysical importance of binary star systems, detections are limited to those located in small ranges of separations, distances, and masses and thus it is necessary to use a variety of observational techniques for a complete view of stellar multiplicity across a broad range of physical parameters. In this paper, we report the detections and measurements of two binaries discovered from observations of microlensing events MOA-2011-BLG-090 and OGLE-2011-BLG-0417. Determinations of the binary masses are possible by simultaneously measuring the Einstein radius and the lens parallax. The measured masses of the binary components are 0.43 M⊙ and 0.39 M⊙ for MOA-2011-BLG-090 and 0.57 M⊙ and 0.17 M⊙ for OGLE-2011-BLG-0417 and thus both lens components of MOA-2011-BLG-090 and one component of OGLE-2011-BLG-0417 are M dwarfs, demonstrating the usefulness of microlensing in detecting binaries composed of low-mass components. From modeling of the light curves considering full Keplerian motion of the lens, we also measure the orbital parameters of the binaries. The blended light of OGLE-2011-BLG-0417 comes very likely from the lens itself, making it possible to check the microlensing orbital solution by follow-up radial-velocity observation. For both events, the caustic-crossing parts of the light curves, which are critical for determining the physical lens parameters, were resolved by high-cadence survey observations and thus it is expected that the number of microlensing binaries with measured physical parameters will increase in the future.

Published
2012

104. First Geodetic Observations Using New VLBI Stations ASKAP-29 and WARK12M

Author

Petrov, L., Phillips, C., Tzioumis, T., Stansby, Bruce, Reynolds, Cormac, Bignall, Hayley, Gulyaev, S., Natusch, T., Palmer, N., Collett, D., Reynolds, J., Amy, S., Wayth, Randall, Tingay, Steven, Petrov, L., Phillips, C., Tzioumis, T., Stansby, Bruce, Reynolds, Cormac, Bignall, Hayley, Gulyaev, S., Natusch, T., Palmer, N., Collett, D., Reynolds, J., Amy, S., Wayth, Randall, and Tingay, Steven

Abstract

We report the results of a successful 7-hour 1.4 GHz Very Long Baseline Interferometry (VLBI) experiment using two new stations, ASKAP-29 located in Western Australia and WARK12M located on the North Island of New Zealand. This was the first geodetic VLBI observing session with the participation of these new stations. We have determined the positions of ASKAP-29 and WARK12M. Random errors on position estimates are 150–200mm for the vertical component and 40–50mm for the horizontal component. Systematic errors caused by the unmodeled ionosphere path delay may reach 1.3mfor the vertical component.

Published
2011

105. Evolution of the parsec-scale structure of PKS 1934-638 revisited: first science with the ASKAP and New Zealand telescopes

Author

Tzioumis, A.K., Tingay, Steven, Stansby, Bruce, Reynolds, J.E., Phillips, C.J., Amy, S.W., Edwards, P.G., Bowen, M.A., Leach, M., Kesteven, M., Chung, Y., Stevens, J., Forsyth, A., Gulyaev, S., Natusch, T., Macquart, Jean-Pierre, Reynolds, Cormac, Wayth, R., Bignall, Hayley, Hotan, Aidan, Hotan, C., Godfrey, L., Ellingsen, S., Dickey, J., Blanchard, J., Lovell, J.E.J., Tzioumis, A.K., Tingay, Steven, Stansby, Bruce, Reynolds, J.E., Phillips, C.J., Amy, S.W., Edwards, P.G., Bowen, M.A., Leach, M., Kesteven, M., Chung, Y., Stevens, J., Forsyth, A., Gulyaev, S., Natusch, T., Macquart, Jean-Pierre, Reynolds, Cormac, Wayth, R., Bignall, Hayley, Hotan, Aidan, Hotan, C., Godfrey, L., Ellingsen, S., Dickey, J., Blanchard, J., and Lovell, J.E.J.

Published
2010

106. A giant planet beyond the snow line in microlensing event OGLE-2011-BLG-0251

Author

Kains, N., primary, Street, R. A., additional, Choi, J.-Y., additional, Han, C., additional, Udalski, A., additional, Almeida, L. A., additional, Jablonski, F., additional, Tristram, P. J., additional, Jørgensen, U. G., additional, Szymański, M. K., additional, Kubiak, M., additional, Pietrzyński, G., additional, Soszyński, I., additional, Poleski, R., additional, Kozłowski, S., additional, Pietrukowicz, P., additional, Ulaczyk, K., additional, Wyrzykowski, Ł., additional, Skowron, J., additional, Alsubai, K. A., additional, Bozza, V., additional, Browne, P., additional, Burgdorf, M. J., additional, Calchi Novati, S., additional, Dodds, P., additional, Dominik, M., additional, Dreizler, S., additional, Fang, X.-S., additional, Grundahl, F., additional, Gu, C.-H., additional, Hardis, S., additional, Harpsøe, K., additional, Hessman, F. V., additional, Hinse, T. C., additional, Hornstrup, A., additional, Hundertmark, M., additional, Jessen-Hansen, J., additional, Kerins, E., additional, Liebig, C., additional, Lund, M., additional, Lundkvist, M., additional, Mancini, L., additional, Mathiasen, M., additional, Penny, M. T., additional, Rahvar, S., additional, Ricci, D., additional, Sahu, K. C., additional, Scarpetta, G., additional, Skottfelt, J., additional, Snodgrass, C., additional, Southworth, J., additional, Surdej, J., additional, Tregloan-Reed, J., additional, Wambsganss, J., additional, Wertz, O., additional, Bajek, D., additional, Bramich, D. M., additional, Horne, K., additional, Ipatov, S., additional, Steele, I. A., additional, Tsapras, Y., additional, Abe, F., additional, Bennett, D. P., additional, Bond, I. A., additional, Botzler, C. S., additional, Chote, P., additional, Freeman, M., additional, Fukui, A., additional, Furusawa, K., additional, Itow, Y., additional, Ling, C. H., additional, Masuda, K., additional, Matsubara, Y., additional, Miyake, N., additional, Muraki, Y., additional, Ohnishi, K., additional, Rattenbury, N., additional, Saito, T., additional, Sullivan, D. J., additional, Sumi, T., additional, Suzuki, D., additional, Suzuki, K., additional, Sweatman, W. L., additional, Takino, S., additional, Wada, K., additional, Yock, P. C. M., additional, Allen, W., additional, Batista, V., additional, Chung, S.-J., additional, Christie, G., additional, DePoy, D. L., additional, Drummond, J., additional, Gaudi, B. S., additional, Gould, A., additional, Henderson, C., additional, Jung, Y.-K., additional, Koo, J.-R., additional, Lee, C.-U., additional, McCormick, J., additional, McGregor, D., additional, Muñoz, J. A., additional, Natusch, T., additional, Ngan, H., additional, Park, H., additional, Pogge, R. W., additional, Shin, I.-G., additional, Yee, J., additional, Albrow, M. D., additional, Bachelet, E., additional, Beaulieu, J.-P., additional, Brillant, S., additional, Caldwell, J. A. R., additional, Cassan, A., additional, Cole, A., additional, Corrales, E., additional, Coutures, Ch., additional, Dieters, S., additional, Dominis Prester, D., additional, Donatowicz, J., additional, Fouqué, P., additional, Greenhill, J., additional, Kane, S. R., additional, Kubas, D., additional, Marquette, J.-B., additional, Martin, R., additional, Meintjes, P., additional, Menzies, J., additional, Pollard, K. R., additional, Williams, A., additional, Wouters, D., additional, and Zub, M., additional

Published
2013
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107. GRB 091029: at the limit of the fireball scenario

Author

Filgas, R., primary, Greiner, J., additional, Schady, P., additional, de Ugarte Postigo, A., additional, Oates, S. R., additional, Nardini, M., additional, Krühler, T., additional, Panaitescu, A., additional, Kann, D. A., additional, Klose, S., additional, Afonso, P. M. J., additional, Allen, W. H., additional, Castro-Tirado, A. J., additional, Christie, G. W., additional, Dong, S., additional, Elliott, J., additional, Natusch, T., additional, Nicuesa Guelbenzu, A., additional, E., F. Olivares, additional, Rau, A., additional, Rossi, A., additional, Sudilovsky, V., additional, and Yock, P. C. M., additional

Published
2012
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108. EVOLUTION OF THE PARSEC-SCALE STRUCTURE OF PKS 1934–638 REVISITED: FIRST SCIENCE WITH THE ASKAP AND NEW ZEALAND TELESCOPES

Author

Tzioumis, A. K., primary, Tingay, S. J., additional, Stansby, B., additional, Reynolds, J. E., additional, Phillips, C. J., additional, Amy, S. W., additional, Edwards, P. G., additional, Bowen, M. A., additional, Leach, M. R., additional, Kesteven, M. J., additional, Chung, Y., additional, Stevens, J., additional, Forsyth, A. R., additional, Gulyaev, S., additional, Natusch, T., additional, Macquart, J.-P., additional, Reynolds, C., additional, Wayth, R. B., additional, Bignall, H. E., additional, Hotan, A., additional, Hotan, C., additional, Godfrey, L., additional, Ellingsen, S., additional, Dickey, J., additional, Blanchard, J., additional, and Lovell, J. E. J., additional

Published
2010
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109. EXTREME MAGNIFICATION MICROLENSING EVENT OGLE-2008-BLG-279: STRONG LIMITS ON PLANETARY COMPANIONS TO THE LENS STAR

Author

Yee, J. C., primary, Udalski, A., additional, Sumi, T., additional, Dong, Subo, additional, Kozłowski, S., additional, Bird, J. C., additional, Cole, A., additional, Higgins, D., additional, McCormick, J., additional, Monard, L. A. G., additional, Polishook, D., additional, Shporer, A., additional, Spector, O., additional, Szymański, M. K., additional, Kubiak, M., additional, Pietrzyński, G., additional, Soszyński, I., additional, Szewczyk, O., additional, Ulaczyk, K., additional, Wyrzykowski, Ł., additional, Poleski, R., additional, Allen, W., additional, Bos, M., additional, Christie, G. W., additional, DePoy, D. L., additional, Eastman, J. D., additional, Gaudi, B. S., additional, Gould, A., additional, Han, C., additional, Kaspi, S., additional, Lee, C. -U., additional, Mallia, F., additional, Maury, A., additional, Maoz, D., additional, Natusch, T., additional, Park, B. -G., additional, Pogge, R. W., additional, Santallo, R., additional, Abe, F., additional, Bond, I. A., additional, Fukui, A., additional, Furusawa, K., additional, Hearnshaw, J. B., additional, Hosaka, S., additional, Itow, Y., additional, Kamiya, K., additional, Korpela, A. V., additional, Kilmartin, P. M., additional, Lin, W., additional, Ling, C. H., additional, Makita, S., additional, Masuda, K., additional, Matsubara, Y., additional, Miyake, N., additional, Muraki, Y., additional, Nagaya, M., additional, Nishimoto, K., additional, Ohnishi, K., additional, Perrott, Y. C., additional, Rattenbury, N. J., additional, Sako, T., additional, Saito, To., additional, Skuljan, L., additional, Sullivan, D. J., additional, Sweatman, W. L., additional, Tristram, P. J., additional, Yock, P. C. M., additional, Albrow, M. D., additional, Batista, V., additional, Fouqué, P., additional, Beaulieu, J. -P., additional, Bennett, D. P., additional, Cassan, A., additional, Comparat, J., additional, Coutures, C., additional, Dieters, S., additional, Greenhill, J., additional, Horne, K., additional, Kains, N., additional, Kubas, D., additional, Martin, R., additional, Menzies, J., additional, Wambsganss, J., additional, Williams, A., additional, and Zub, M., additional

Published
2009
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110. VERTICAL STRUCTURE IN PLUTO'S ATMOSPHERE FROM THE 2006 JUNE 12 STELLAR OCCULTATION

Author

Young, E. F., primary, French, R. G., additional, Young, L. A., additional, Ruhland, C. R., additional, Buie, M. W., additional, Olkin, C. B., additional, Regester, J., additional, Shoemaker, K., additional, Blow, G., additional, Broughton, J., additional, Christie, G., additional, Gault, D., additional, Lade, B., additional, and Natusch, T., additional

Published
2008
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113. A brown dwarf orbiting an M-dwarf: MOA 2009-BLG-411L.

Author

Bachelet, E., Fouqué, P., Han, C., Gould, A., Albrow, M. D., Beaulieu, J.-P., Bertin, E., Bond, I. A., Christie, G. W., Heyrovský, D., Horne, K., Jørgensen, U. G., Maoz, D., Mathiasen, M., Matsunaga, N., McCormick, J., Menzies, J., Nataf, D., Natusch, T., and Oi, N.

Subjects
DWARF stars, CAUSTICS (Optics), GIANT stars, INTERSTELLAR medium, ASTRONOMY, ASTROPHYSICS
Abstract

Context. Caustic crossing is the clearest signature of binary lenses in microlensing. In the present context, this signature is diluted by the large source star but a detailed analysis has allowed the companion signal to be extracted. Aims. MOA 2009-BLG-411 was detected on August 5, 2009 by the MOA-Collaboration. Alerted as a high-magnification event, it was sensitive to planets. Suspected anomalies in the light curve were not confirmed by a real-time model, but further analysis revealed small deviations from a single lens extended source fit. Methods. Thanks to observations by all the collaborations, this event was well monitored. We first decided to characterize the source star properties by using a more refined method than the classical one: we measure the interstellar absorption along the line of sight in five different passbands (VIJHK). Secondly, we model the lightcurve by using the standard technique: make (s, q, α) grids to look for local minima and refine the results by using a downhill method (Markov chain Monte Carlo). Finally, we use a Galactic model to estimate the physical properties of the lens components. Results. We find that the source star is a giant G star with radius 9 R☉. The grid search gives two local minima, which correspond to the theoretical degeneracy s ≡ s-1. We find that the lens is composed of a brown dwarf secondary of mass MS = 0.05 M☉ orbiting a primary M-star of mass MP = 0.18 M☉. We also reveal a new mass-ratio degeneracy for the central caustics of close binaries. Conclusions. As far as we are aware, this is the first detection using the microlensing technique of a binary system in our Galaxy composed of an M-star and a brown dwarf [ABSTRACT FROM AUTHOR]

Published
2012
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114. VizieR Online Data Catalog: Dynamic SEDs of southern blazars - DSSB (Krauss+, 2016)

Author

Krauss, F., Wilms, J., Matthias Kadler, Ojha, R., Schulz, R., Trustedt, J., Edwards, P. G., Stevens, J., Ros, E., Baumgartner, W., Beuchert, T., Blanchard, J., Buson, S., Carpenter, B., Dauser, T., Falkner, S., Gehrels, N., Grafe, C., Gulyaev, S., Hase, H., Horiuchi, S., Kreikenbohm, A., Kreykenbohm, I., Langejahn, M., Leiter, K., Lovell, J. E. J., Muller, C., Natusch, T., Nesci, R., Pursimo, T., Phillips, C., Plotz, C., Quick, J., Tzioumis, A. K., and Weston, S.

115. Recent updates on the Maser Monitoring Organisation

Author

Burns, R. A., Kobak, A., Caratti O Garatti, A., Tolmachev, A., Volvach, A., Alakoz, A., Wootten, A., Bisyarina, A., Dzodzomenyo, A., Sobolev, A., Bartkiewicz, A., Aberfelds, A., Stecklum, B., Kramer, B., Macdonald, C., Cyganowski, C., Colomer, F., Miro, C. G., Brogan, C., Li, D., Smits, D., Engels, D., Ladeyschikov, D., Johnstone, D., Elena Popova, Proven-Adzri, E., Den Heever, F., Orosz, G., Surcis, G., Wu, G., Macleod, G., Linz, H., Imai, H., Langevelde, H., Valtts, I., Shmeld, I., Chibueze, J. O., Brand, J., Kumar, J., Green, J., Vorster, J., Eislöffel, J., Kim, J., Sugiyama, K., Menten, K., Immer, K., Sunada, K., Kim, K. -T, Volvach, L., Moscadelli, L., Jordan, L., Uscanga, L., Gray, M., Szymczak, M., Olech, M., Hoare, M., Durjasz, M., Uchiyama, M., Shakhvorostova, N., Bayandina, O., Wolak, P., Gulyaev, S., Khaibrakhmanov, S., Breen, S., Goedhart, S., Casu, S., Ellingsen, S., Kurtz, S., Weston, S., Yoshihiro, T., Natusch, T., Hunter, T., Hirota, T., Baan, W., Vlemmings, W., Chen, X., Gong, Y., Yonekura, Y., Szabó, Z. M., Abraham, Z., ITA, USA, GBR, FRA, DEU, ESP, AUS, CAN, KOR, JPN, CHN, and RUS

Abstract

The Maser Monitoring Organisation (M2O) is a research community of telescope operators, astronomy researchers and maser theoreticians pursuing a joint goal of reaching a deeper understanding of maser emission and exploring its variety of uses as tracers of astrophysical events. These proceedings detail the origin, motivations and current status of the M2O, as was introduced at the 2021 EVN symposium.

116. OGLE-2017-BLG-1186: first application of asteroseismology and Gaussian processes to microlensing

Author

Li, S-S, Zang, W, Udalski, A, Shvartzvald, Y, Huber, D, Lee, C-U, Sumi, T, Gould, A, Mao, S, Fouqué, P, Wang, T, Dong, S, Jørgensen, U G, Cole, A, Mróz, P, Szymański, M K, Skowron, J, Poleski, R, Soszyński, I, Pietrukowicz, P, Kozłowski, S, Ulaczyk, K, Rybicki, K A, Iwanek, P, Yee, J C, Novati, S Calchi, Beichman, C A, Bryden, G, Carey, S, Gaudi, B S, Henderson, C B, Zhu, W, Albrow, M D, Chung, S-J, Han, C, Hwang, K-H, Jung, Y K, Ryu, Y-H, Shin, I-G, Cha, S-M, Kim, D-J, Kim, H-W, Kim, S-L, Lee, D-J, Lee, Y, Park, B-G, Pogge, R W, Bond, I A, Abe, F, Barry, R, Bennett, D P, Bhattacharya, A, Donachie, M, Fukui, A, Hirao, Y, Itow, Y, Kondo, I, Koshimoto, N, Li, M C A, Matsubara, Y, Muraki, Y, Miyazaki, S, Nagakane, M, Ranc, C, Rattenbury, N J, Suematsu, H, Sullivan, D J, Suzuki, D, Tristram, P J, Yonehara, A, Christie, G, Drummond, J, Green, J, Hennerley, S, Natusch, T, Porritt, I, Bachelet, E, Maoz, D, Street, R A, Tsapras, Y, Bozza, V, Dominik, M, Hundertmark, M, Peixinho, N, Sajadian, S, Burgdorf, M J, Evans, D F, Jaimes, R Figuera, Fujii, Y I, Haikala, L K, Helling, C, Henning, T, Hinse, T C, Mancini, L, Longa-Pe na, P, Rahvar, S, Rabus, M, Skottfelt, J., Snodgrass, C., Southworth, J, Unda-Sanzana, E, Essen, C von, Beaulieu, J-P, Blackman, J, Hill, K, Li, S-S, Zang, W, Udalski, A, Shvartzvald, Y, Huber, D, Lee, C-U, Sumi, T, Gould, A, Mao, S, Fouqué, P, Wang, T, Dong, S, Jørgensen, U G, Cole, A, Mróz, P, Szymański, M K, Skowron, J, Poleski, R, Soszyński, I, Pietrukowicz, P, Kozłowski, S, Ulaczyk, K, Rybicki, K A, Iwanek, P, Yee, J C, Novati, S Calchi, Beichman, C A, Bryden, G, Carey, S, Gaudi, B S, Henderson, C B, Zhu, W, Albrow, M D, Chung, S-J, Han, C, Hwang, K-H, Jung, Y K, Ryu, Y-H, Shin, I-G, Cha, S-M, Kim, D-J, Kim, H-W, Kim, S-L, Lee, D-J, Lee, Y, Park, B-G, Pogge, R W, Bond, I A, Abe, F, Barry, R, Bennett, D P, Bhattacharya, A, Donachie, M, Fukui, A, Hirao, Y, Itow, Y, Kondo, I, Koshimoto, N, Li, M C A, Matsubara, Y, Muraki, Y, Miyazaki, S, Nagakane, M, Ranc, C, Rattenbury, N J, Suematsu, H, Sullivan, D J, Suzuki, D, Tristram, P J, Yonehara, A, Christie, G, Drummond, J, Green, J, Hennerley, S, Natusch, T, Porritt, I, Bachelet, E, Maoz, D, Street, R A, Tsapras, Y, Bozza, V, Dominik, M, Hundertmark, M, Peixinho, N, Sajadian, S, Burgdorf, M J, Evans, D F, Jaimes, R Figuera, Fujii, Y I, Haikala, L K, Helling, C, Henning, T, Hinse, T C, Mancini, L, Longa-Pe na, P, Rahvar, S, Rabus, M, Skottfelt, J., Snodgrass, C., Southworth, J, Unda-Sanzana, E, Essen, C von, Beaulieu, J-P, Blackman, J, and Hill, K

Abstract

We present the analysis of the event OGLE-2017-BLG-1186 from the 2017 Spitzer microlensing campaign. This is a remarkable microlensing event because its source is photometrically bright and variable, which makes it possible to perform an asteroseismic analysis using ground-based data. We find that the source star is an oscillating red giant with average timescale of ∼9 days. The asteroseismic analysis also provides us source properties including the source angular size (∼27μas) and distance (∼11.5 kpc), which are essential for inferring the properties of the lens. When fitting the light curve, we test the feasibility of Gaussian Processes (GPs) in handling the correlated noise caused by the variable source. We find that the parameters from the GP model are generally more loosely constrained than those from the traditional χ2 minimization method. We note that this event is the first microlensing system for which asteroseismology and GPs have been used to account for the variable source. With both finite-source effect and microlens parallax measured, we find that the lens is likely a ∼0.045 M⊙ brown dwarf at distance ∼9.0 kpc, or a ∼0.073 M⊙ ultracool dwarf at distance ∼9.8 kpc. Combining the estimated lens properties with a Bayesian analysis using a Galactic model, we find a 35% probability for the lens to be a bulge object and 65% to be a background disk object.

117. OGLE-2013-BLG-0911Lb: A Secondary on the Brown-dwarf Planet Boundary around an M Dwarf

Author

Miyazaki, Shota, Sumi, Takahiro, Bennett, David P., Udalski, Andrzej, Shvartzvald, Yossi, Street, Rachel, Bozza, Valerio, Yee, Jennifer C., Bond, Ian A., Rattenbury, Nicholas, Koshimoto, Naoki, Suzuki, Daisuke, Fukui, Akihiko, Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fujii, H., Hirao, Y., Itow, Y., Kamei, Y., Kondo, I., Li, M. C. A., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Sullivan, D. J., Tristram, P. J., Yamakawa, T., Yonehara, A., Skowron, J., Poleski, R., Mróz, P., Szymański, M. K., Soszyński, I., Pietrukowicz, P., KozŁowski, S., Ulaczyk, K., Wyrzykowski, Ł., Friedmann, Matan, Kaspi, Shai, Maoz, Dan, Albrow, M., Christie, G., DePoy, D. L., Gal-Yam, A., Gould, A., Lee, C.-U., Manulis, I., McCormick, J., Natusch, T., Ngan, H., Pogge, R. W., Porritt, I., Tsapras, Y., Bachelet, E., Hundertmark, M. P. G., Dominik, M., Bramich, D. M., Cassan, A., Jaimes, R. Figuera, Horne, K., Schmidt, R., Snodgrass, C., Wambsganss, J., Steele, I. A., Menzies, J., Mao, S., Jø rgensen, U. G., Burgdorf, M. J., Ciceri, S., Novati, S. Calchi, D’Ago, G., Evans, D. F., Hinse, T. C., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Popovas, A., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Peixinho, N., Verma, P., Miyazaki, Shota, Sumi, Takahiro, Bennett, David P., Udalski, Andrzej, Shvartzvald, Yossi, Street, Rachel, Bozza, Valerio, Yee, Jennifer C., Bond, Ian A., Rattenbury, Nicholas, Koshimoto, Naoki, Suzuki, Daisuke, Fukui, Akihiko, Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fujii, H., Hirao, Y., Itow, Y., Kamei, Y., Kondo, I., Li, M. C. A., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Sullivan, D. J., Tristram, P. J., Yamakawa, T., Yonehara, A., Skowron, J., Poleski, R., Mróz, P., Szymański, M. K., Soszyński, I., Pietrukowicz, P., KozŁowski, S., Ulaczyk, K., Wyrzykowski, Ł., Friedmann, Matan, Kaspi, Shai, Maoz, Dan, Albrow, M., Christie, G., DePoy, D. L., Gal-Yam, A., Gould, A., Lee, C.-U., Manulis, I., McCormick, J., Natusch, T., Ngan, H., Pogge, R. W., Porritt, I., Tsapras, Y., Bachelet, E., Hundertmark, M. P. G., Dominik, M., Bramich, D. M., Cassan, A., Jaimes, R. Figuera, Horne, K., Schmidt, R., Snodgrass, C., Wambsganss, J., Steele, I. A., Menzies, J., Mao, S., Jø rgensen, U. G., Burgdorf, M. J., Ciceri, S., Novati, S. Calchi, D’Ago, G., Evans, D. F., Hinse, T. C., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Popovas, A., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Peixinho, N., and Verma, P.

Abstract

We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q $\simeq$ 0.03, which differs from that reported in Shvartzvald et al. The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s ∼ 0.15 or s ∼ 7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M dwarf orbited by a massive Jupiter companion at very close (${M}_{\mathrm{host}}={0.30}_{-0.06}^{+0.08}{M}_{\odot }$, ${M}_{\mathrm{comp}}={10.1}_{-2.2}^{+2.9}{M}_{\mathrm{Jup}}$, ${a}_{\exp }={0.40}_{-0.04}^{+0.05}\,\mathrm{au}$) or wide (${M}_{\mathrm{host}}={0.28}_{-0.08}^{+0.10}{M}_{\odot }$, ${M}_{\mathrm{comp}}={9.9}_{-3.5}^{+3.8}{M}_{\mathrm{Jup}}$, ${a}_{\exp }={18.0}_{-3.2}^{+3.2}\,\mathrm{au}$) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q = 0.03, which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13M$_{Jup}$. It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ∼13M$_{Jup}$ in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M dwarfs and even BDs, which is challenging for other exoplanet detection methods.

118. Precision measurement of a brown dwarf mass in a binary system in the microlensing event

Author

Herald, A., Udalski, A., Bozza, V., Rota, P., Bond, I. A., Yee, J. C., Sajadian, S., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Pietrukowicz, P., Kozłowski, S., Ulaczyk, K., Rybicki, K. A., Iwanek, P., Wrona, M., Gromadzki, M., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Fukui, A., Fujii, H., Hirao, Y., Itow, Y., Kirikawa, R., Kondo, I., Koshimoto, N., Matsubara, Y., Matsumoto, S., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Okamura, A., Rattenbury, N. J., Satoh, Y., Sumi, T., Suzuki, D., Silva, S. Ishitani, Toda, T., Tristram, P. J., Vandorou, A., Yama, H., Beichman, C. A., Bryden, G., Novati, S. Calchi, Carey, S., Gaudi, B. S., Gould, A., Henderson, C. B., Johnson, S., Shvartzvald, Y., Zhu, W., Dominik, M., Hundertmark, M., Jørgensen, U. G., Longa-Peña, P., Skottfelt, J., Tregloan-Reed, J., Bach-Møller, N., Burgdorf, M., D’Ago, G., Haikala, L., Hitchcock, J., Khalouei, E., Peixinho, N., Rahvar, S., Snodgrass, C., Southworth, J., Spyratos, P., Zang, W., Yang, H., Mao, S., Bachelet, E., Maoz, D., Street, R. A., Tsapras, Y., Christie, G. W., Cooper, T., de Almeida, L., do Nascimento, J.-D., Green, J., Han, C., Hennerley, S., Marmont, A., McCormick, J., Monard, L. A. G., Natusch, T., Pogge, R., Herald, A., Udalski, A., Bozza, V., Rota, P., Bond, I. A., Yee, J. C., Sajadian, S., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Pietrukowicz, P., Kozłowski, S., Ulaczyk, K., Rybicki, K. A., Iwanek, P., Wrona, M., Gromadzki, M., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Fukui, A., Fujii, H., Hirao, Y., Itow, Y., Kirikawa, R., Kondo, I., Koshimoto, N., Matsubara, Y., Matsumoto, S., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Okamura, A., Rattenbury, N. J., Satoh, Y., Sumi, T., Suzuki, D., Silva, S. Ishitani, Toda, T., Tristram, P. J., Vandorou, A., Yama, H., Beichman, C. A., Bryden, G., Novati, S. Calchi, Carey, S., Gaudi, B. S., Gould, A., Henderson, C. B., Johnson, S., Shvartzvald, Y., Zhu, W., Dominik, M., Hundertmark, M., Jørgensen, U. G., Longa-Peña, P., Skottfelt, J., Tregloan-Reed, J., Bach-Møller, N., Burgdorf, M., D’Ago, G., Haikala, L., Hitchcock, J., Khalouei, E., Peixinho, N., Rahvar, S., Snodgrass, C., Southworth, J., Spyratos, P., Zang, W., Yang, H., Mao, S., Bachelet, E., Maoz, D., Street, R. A., Tsapras, Y., Christie, G. W., Cooper, T., de Almeida, L., do Nascimento, J.-D., Green, J., Han, C., Hennerley, S., Marmont, A., McCormick, J., Monard, L. A. G., Natusch, T., and Pogge, R.

Abstract

Context Brown dwarfs are transition objects between stars and planets that are still poorly understood, for which several competing mechanisms have been proposed to describe their formation. Mass measurements are generally difficult to carry out for isolated objects as well as for brown dwarfs orbiting low-mass stars, which are often too faint for a spectroscopic follow-up. Aims Microlensing provides an alternative tool for the discovery and investigation of such faint systems. Here, we present an analysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, which is caused by a binary system composed of a brown dwarf orbiting a red dwarf. Methods Thanks to extensive ground observations and the availability of space observations from Spitzer, it has been possible to obtain accurate estimates of all microlensing parameters, including the parallax, source radius, and orbital motion of the binary lens. Results Following an accurate modeling process, we found that the lens is composed of a red dwarf with a mass of M1 = 0.149 ± 0.010 M⊙ and a brown dwarf with a mass of M2 = 0.0463 ± 0.0031 M⊙at a projected separation of a⊥ = 0.585 au. The system has a peculiar velocity that is typical of old metal-poor populations in the thick disk. A percent-level precision in the mass measurement of brown dwarfs has been achieved only in a few microlensing events up to now, but will likely become more common in the future thanks to the Roman space telescope.

119. OGLE-2013-BLG-0911Lb: A Secondary on the Brown-dwarf Planet Boundary around an M Dwarf

Author

Miyazaki, Shota, Sumi, Takahiro, Bennett, David P., Udalski, Andrzej, Shvartzvald, Yossi, Street, Rachel, Bozza, Valerio, Yee, Jennifer C., Bond, Ian A., Rattenbury, Nicholas, Koshimoto, Naoki, Suzuki, Daisuke, Fukui, Akihiko, Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fujii, H., Hirao, Y., Itow, Y., Kamei, Y., Kondo, I., Li, M. C. A., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Sullivan, D. J., Tristram, P. J., Yamakawa, T., Yonehara, A., Skowron, J., Poleski, R., Mróz, P., Szymański, M. K., Soszyński, I., Pietrukowicz, P., KozŁowski, S., Ulaczyk, K., Wyrzykowski, Ł., Friedmann, Matan, Kaspi, Shai, Maoz, Dan, Albrow, M., Christie, G., DePoy, D. L., Gal-Yam, A., Gould, A., Lee, C.-U., Manulis, I., McCormick, J., Natusch, T., Ngan, H., Pogge, R. W., Porritt, I., Tsapras, Y., Bachelet, E., Hundertmark, M. P. G., Dominik, M., Bramich, D. M., Cassan, A., Jaimes, R. Figuera, Horne, K., Schmidt, R., Snodgrass, C., Wambsganss, J., Steele, I. A., Menzies, J., Mao, S., Jø rgensen, U. G., Burgdorf, M. J., Ciceri, S., Novati, S. Calchi, D’Ago, G., Evans, D. F., Hinse, T. C., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Popovas, A., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Peixinho, N., Verma, P., Miyazaki, Shota, Sumi, Takahiro, Bennett, David P., Udalski, Andrzej, Shvartzvald, Yossi, Street, Rachel, Bozza, Valerio, Yee, Jennifer C., Bond, Ian A., Rattenbury, Nicholas, Koshimoto, Naoki, Suzuki, Daisuke, Fukui, Akihiko, Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fujii, H., Hirao, Y., Itow, Y., Kamei, Y., Kondo, I., Li, M. C. A., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Sullivan, D. J., Tristram, P. J., Yamakawa, T., Yonehara, A., Skowron, J., Poleski, R., Mróz, P., Szymański, M. K., Soszyński, I., Pietrukowicz, P., KozŁowski, S., Ulaczyk, K., Wyrzykowski, Ł., Friedmann, Matan, Kaspi, Shai, Maoz, Dan, Albrow, M., Christie, G., DePoy, D. L., Gal-Yam, A., Gould, A., Lee, C.-U., Manulis, I., McCormick, J., Natusch, T., Ngan, H., Pogge, R. W., Porritt, I., Tsapras, Y., Bachelet, E., Hundertmark, M. P. G., Dominik, M., Bramich, D. M., Cassan, A., Jaimes, R. Figuera, Horne, K., Schmidt, R., Snodgrass, C., Wambsganss, J., Steele, I. A., Menzies, J., Mao, S., Jø rgensen, U. G., Burgdorf, M. J., Ciceri, S., Novati, S. Calchi, D’Ago, G., Evans, D. F., Hinse, T. C., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Popovas, A., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Peixinho, N., and Verma, P.

Abstract

We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q $\simeq$ 0.03, which differs from that reported in Shvartzvald et al. The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s ∼ 0.15 or s ∼ 7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M dwarf orbited by a massive Jupiter companion at very close (${M}_{\mathrm{host}}={0.30}_{-0.06}^{+0.08}{M}_{\odot }$, ${M}_{\mathrm{comp}}={10.1}_{-2.2}^{+2.9}{M}_{\mathrm{Jup}}$, ${a}_{\exp }={0.40}_{-0.04}^{+0.05}\,\mathrm{au}$) or wide (${M}_{\mathrm{host}}={0.28}_{-0.08}^{+0.10}{M}_{\odot }$, ${M}_{\mathrm{comp}}={9.9}_{-3.5}^{+3.8}{M}_{\mathrm{Jup}}$, ${a}_{\exp }={18.0}_{-3.2}^{+3.2}\,\mathrm{au}$) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q = 0.03, which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13M$_{Jup}$. It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ∼13M$_{Jup}$ in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M dwarfs and even BDs, which is challenging for other exoplanet detection methods.

120. TANAMI: Tracking Active Galactic Nuclei with Austral Milliarcsecond Interferometry

Author

Müller, C., Kadler, M., Ojha, R., Schulz, R., Trüstedt, J., Edwards, P. G., Ros, E., Carpenter, B., Angioni, R., Blanchard, J., Böck, M., Burd, P. R., Dörr, M., Dutka, M. S., Eberl, T., Gulyaev, S., Hase, H., Horiuchi, S., Katz, U., Krauß, F., Lovell, J. E. J., Natusch, T., Nesci, R., Phillips, C., Plötz, C., Pursimo, T., Quick, J. F. H., Stevens, J., Thompson, D. J., Tingay, S. J., Tzioumis, A. K., Weston, S., Wilms, J., and Zensus, J. A.

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122. Coincidence of a high-fluence blazar outburst with a PeV-energy neutrino event

Author

D. Eisenacher Glawion, Bryce Carpenter, J. A. Zensus, S. Buson, Karl Mannheim, Tim Natusch, Dominik Elsässer, Jamie Stevens, M. Kreter, Julie McEnery, Francesco Longo, Christian Plötz, D. J. Thompson, Chris Phillips, Shinji Horiuchi, E. Litzinger, Felicia Krauß, C. Gräfe, F. W. Stecker, I. Kreykenbohm, Gisela Anton, Alexander Kappes, Thomas Eberl, Philip G. Edwards, T. Beuchert, Eduardo Ros, C. Müller, Jörn Wilms, Sergei Gulyaev, J. Trüstedt, K. Leiter, James E. J. Lovell, Uli Katz, C. W. James, Anastasios Tzioumis, Roopesh Ojha, J. F. H. Quick, T. Steinbring, A. Kreikenbohm, M. Langejahn, Matthias Kadler, Stuart Weston, R. Schulz, W. Baumgartner, N. Gehrels, H. Hase, Kadler, M, Krauß, F., Mannheim, K., Ojha, R., Müller, C., Schulz, R., Anton, G., Baumgartner, W., Beuchert, T., Buson, S., Carpenter, B., Eberl, T., Edwards, P. G., Eisenacher Glawion, D., Elsässer, D., Gehrels, N., Gräfe, C., Gulyaev, S., Hase, H., Horiuchi, S., James, C. W., Kappes, A., Katz, U., Kreikenbohm, A., Kreter, M., Kreykenbohm, I., Langejahn, M., Leiter, K., Litzinger, E., Longo, Francesco, Lovell, J. E. J., Mcenery, J., Natusch, T., Phillips, C., Plötz, C., Quick, J., Ros, E., Stecker, F. W., Steinbring, T., Stevens, J., Thompson, D. J., Trüstedt, J., Tzioumis, A. K., Weston, S., Wilms, J., and Zensus, J. A.

Subjects
High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Neutrino telescope, FOS: Physical sciences, General Physics and Astronomy, Physics and Astronomy, Neutrino, Active Galactic Nuclei, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Fluence, Coincidence, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, High Energy Physics - Phenomenology, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - High Energy Astrophysical Phenomena, Event (particle physics)
Abstract

The discovery of extraterrestrial very-high-energy neutrinos by the IceCube collaboration has launched a quest for the identification of their astrophysical sources. Gamma-ray blazars have been predicted to yield a cumulative neutrino signal exceeding the atmospheric background above energies of 100 TeV, assuming that both the neutrinos and the gamma-ray photons are produced by accelerated protons in relativistic jets. Since the background spectrum falls steeply with increasing energy, the individual events with the clearest signature of being of an extraterrestrial origin are those at PeV energies. Inside the large positional-uncertainty fields of the first two PeV neutrinos detected by IceCube, the integrated emission of the blazar population has a sufficiently high electromagnetic flux to explain the detected IceCube events, but fluences of individual objects are too low to make an unambiguous source association. Here, we report that a major outburst of the blazar PKS B1424-418 occurred in temporal and positional coincidence with the third PeV-energy neutrino event (IC35) detected by IceCube. Based on an analysis of the full sample of gamma-ray blazars in the IC35 field and assuming a photo-hadronic emission model, we show that the long-term average gamma-ray emission of blazars as a class is in agreement with both the measured all-sky flux of PeV neutrinos and the spectral slope of the IceCube signal. The outburst of PKS B1424-418 has provided an energy output high enough to explain the observed PeV event, indicative of a direct physical association., Accepted for publication in Nature Physics on Mar 3rd, 2016 (arXiv version is the original submitted manuscript as per NatPhys regulations), 38 pages (including 10 pages of supplementary material), 3 figures

Published
2016

123. GRB 091029: at the limit of the fireball scenario

Author

R. Filgas, J. Greiner, P. Schady, A. de Ugarte Postigo, S. R. Oates, M. Nardini, T. Krühler, A. Panaitescu, D. A. Kann, S. Klose, P. M. J. Afonso, W. H. Allen, A. J. Castro-Tirado, G. W. Christie, S. Dong, J. Elliott, T. Natusch, A. Nicuesa Guelbenzu, F. Olivares E., A. Rau, A. Rossi, V. Sudilovsky, P. C. M. Yock, Filgas, R, Greiner, J, Schady, P, de Ugarte Postigo, A, Oates, S, Nardini, M, Krühler, T, Panaitescu, A, Kann, D, Klose, S, Afonso, P, Allen, W, Castro Tirado, A, Christie, G, Dong, S, Elliott, J, Natusch, T, Nicuesa Guelbenzu, A, E., F, Rau, A, Rossi, A, Sudilovsky, V, and Yock, P

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Swift Gamma-Ray Burst Mission, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma rays: ISM, gamma-ray burst: individual: GRB 091029, ISM: jets and outflows, X-rays: individuals: GRB 091029, Light curve, Afterglow, FIS/05 - ASTRONOMIA E ASTROFISICA, Space and Planetary Science, Outflow, Limit (mathematics), Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Energy (signal processing), Free parameter
Abstract

Using high-quality, broad-band afterglow data for GRB 091029, we test the validity of the forward-shock model for gamma-ray burst afterglows. We used multi-wavelength (NIR to X-ray) follow-up observations obtained with the GROND, BOOTES-3/YA and Stardome optical ground-based telescopes, and the UVOT and the XRT onboard the Swift satellite. To explain the almost totally decoupled light curves in the X-ray and optical/NIR domains, a two-component outflow is proposed. Several models are tested, including continuous energy injection, components with different electron energy indices and components in two different stages of spectral evolution. Only the last model can explain both the decoupled light curves with asynchronous peaks and the peculiar SED evolution. However, this model has so many unknown free parameters that we are unable to reliably confirm or disprove its validity, making the afterglow of GRB 091029 difficult to explain in the framework of the simplest fireball model., Comment: Accepted to A&A

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