The Experts below are selected from a list of 37626 Experts worldwide ranked by ideXlab platform
Daniella Bardalez C Gagliuffi - One of the best experts on this subject based on the ideXlab platform.
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radio emission and Orbital Motion from the close encounter star brown dwarf binary wise j072003 20 084651 2
The Astronomical Journal, 2015Co-Authors: Adam J Burgasser, Carl Melis, Jacob Todd, Christopher R Gelino, Gregg Hallinan, Daniella Bardalez C GagliuffiAbstract:We report the detection of radio emission and Orbital Motion from the nearby star–brown dwarf binary WISE J072003.20–084651.2AB. Radio observations across the 4.5–6.5 GHz band with the Very Large Array identify at the position of the system quiescent emission with a flux density of 15 ± 3 μJy, and a highly polarized radio source that underwent a 2–3 minute burst with peak flux density 300 ± 90 μJy. The latter emission is likely a low-level magnetic flare similar to optical flares previously observed for this source. No outbursts were detected in separate narrow-band Hα monitoring observations. We report new high-resolution imaging and spectroscopic observations that confirm the presence of a co-moving T5.5 secondary and provide the first indications of three-dimensional Orbital Motion. We used these data to revise our estimates for the Orbital period (4.1_(-1.3)^(+2.7) year) and tightly constrain the Orbital inclination to be nearly edge-on (93o6^(+1o6)_(−1o4)), although robust measures of the component and system masses will require further monitoring. The inferred Orbital Motion does not change the high likelihood that this radio-emitting very low-mass binary made a close pass to the Sun in the past 100 kyr.
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radio emission and Orbital Motion from the close encounter star brown dwarf binary wise j072003 20 084651 2
arXiv: Solar and Stellar Astrophysics, 2015Co-Authors: Adam J Burgasser, Carl Melis, Jacob Todd, Christopher R Gelino, Gregg Hallinan, Daniella Bardalez C GagliuffiAbstract:We report the detection of radio emission and Orbital Motion from the nearby star-brown dwarf binary WISE J072003.20-084651.2AB. Radio observations across the 4.5-6.5 GHz band with the Very Large Array identify at the position of the system quiescent emission with a flux density of 15$\pm$3 $\mu$Jy, and a highly-polarized radio source that underwent a 2-3 min burst with peak flux density 300$\pm$90 $\mu$Jy. The latter emission is likely a low-level magnetic flare similar to optical flares previously observed for this source. No outbursts were detected in separate narrow-band H$\alpha$ monitoring observations. We report new high-resolution imaging and spectroscopic observations that confirm the presence of a co-moving T5.5 secondary and provide the first indications of three-dimensional Orbital Motion. We used these data to revise our estimates for the Orbital period (4.1$^{+2.7}_{-1.3}$ yr) and tightly constrain the Orbital inclination to be nearly edge-on (93.6\deg$^{+1.6\deg}_{-1.4\deg}$), although robust measures of the component and system masses will require further monitoring. The inferred Orbital Motion does not change the high likelihood that this radio-emitting very low-mass binary made a close pass to the Sun in the past 100 kyr.
Jennifer Patience - One of the best experts on this subject based on the ideXlab platform.
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Orbital Motion in pre main sequence binaries
The Astronomical Journal, 2014Co-Authors: Gail H Schaefer, L Prato, M Simon, Jennifer PatienceAbstract:We present results from our ongoing program to map the visual orbits of pre-main sequence (PMS) binaries in the Taurus star forming region using adaptive optics imaging at the Keck Observatory. We combine our results with measurements reported in the literature to analyze the Orbital Motion for each binary. We present preliminary orbits for DF Tau, T Tau S, ZZ Tau, and the Pleiades binary HBC 351. Seven additional binaries show curvature in their relative Motion. Currently, we can place lower limits on the Orbital periods for these systems; full solutions will be possible with more Orbital coverage. Five other binaries show Motion that is indistinguishable from linear Motion. We suspect that these systems are bound and might show curvature with additional measurements in the future. The observations reported herein lay critical groundwork toward the goal of measuring precise masses for low-mass PMS stars.
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Orbital Motion in pre main sequence binaries
arXiv: Solar and Stellar Astrophysics, 2014Co-Authors: Gail H Schaefer, L Prato, M Simon, Jennifer PatienceAbstract:We present results from our ongoing program to map the visual orbits of pre-main sequence binaries in the Taurus star forming region using adaptive optics imaging at the Keck Observatory. We combine our results with measurements reported in the literature to analyze the Orbital Motion for each binary. We present preliminary orbits for DF Tau, T Tau S, ZZ Tau, and the Pleiades binary HBC 351. Seven additional binaries show curvature in their relative Motion. Currently, we can place lower limits on the Orbital periods for these systems; full solutions will be possible with more Orbital coverage. Five other binaries show Motion that is indistinguishable from linear Motion. We suspect that these systems are bound and might show curvature with additional measurements in the future. The observations reported herein lay critical groundwork toward the goal of measuring precise masses for low-mass pre-main sequence stars.
Adam J Burgasser - One of the best experts on this subject based on the ideXlab platform.
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radio emission and Orbital Motion from the close encounter star brown dwarf binary wise j072003 20 084651 2
The Astronomical Journal, 2015Co-Authors: Adam J Burgasser, Carl Melis, Jacob Todd, Christopher R Gelino, Gregg Hallinan, Daniella Bardalez C GagliuffiAbstract:We report the detection of radio emission and Orbital Motion from the nearby star–brown dwarf binary WISE J072003.20–084651.2AB. Radio observations across the 4.5–6.5 GHz band with the Very Large Array identify at the position of the system quiescent emission with a flux density of 15 ± 3 μJy, and a highly polarized radio source that underwent a 2–3 minute burst with peak flux density 300 ± 90 μJy. The latter emission is likely a low-level magnetic flare similar to optical flares previously observed for this source. No outbursts were detected in separate narrow-band Hα monitoring observations. We report new high-resolution imaging and spectroscopic observations that confirm the presence of a co-moving T5.5 secondary and provide the first indications of three-dimensional Orbital Motion. We used these data to revise our estimates for the Orbital period (4.1_(-1.3)^(+2.7) year) and tightly constrain the Orbital inclination to be nearly edge-on (93o6^(+1o6)_(−1o4)), although robust measures of the component and system masses will require further monitoring. The inferred Orbital Motion does not change the high likelihood that this radio-emitting very low-mass binary made a close pass to the Sun in the past 100 kyr.
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radio emission and Orbital Motion from the close encounter star brown dwarf binary wise j072003 20 084651 2
arXiv: Solar and Stellar Astrophysics, 2015Co-Authors: Adam J Burgasser, Carl Melis, Jacob Todd, Christopher R Gelino, Gregg Hallinan, Daniella Bardalez C GagliuffiAbstract:We report the detection of radio emission and Orbital Motion from the nearby star-brown dwarf binary WISE J072003.20-084651.2AB. Radio observations across the 4.5-6.5 GHz band with the Very Large Array identify at the position of the system quiescent emission with a flux density of 15$\pm$3 $\mu$Jy, and a highly-polarized radio source that underwent a 2-3 min burst with peak flux density 300$\pm$90 $\mu$Jy. The latter emission is likely a low-level magnetic flare similar to optical flares previously observed for this source. No outbursts were detected in separate narrow-band H$\alpha$ monitoring observations. We report new high-resolution imaging and spectroscopic observations that confirm the presence of a co-moving T5.5 secondary and provide the first indications of three-dimensional Orbital Motion. We used these data to revise our estimates for the Orbital period (4.1$^{+2.7}_{-1.3}$ yr) and tightly constrain the Orbital inclination to be nearly edge-on (93.6\deg$^{+1.6\deg}_{-1.4\deg}$), although robust measures of the component and system masses will require further monitoring. The inferred Orbital Motion does not change the high likelihood that this radio-emitting very low-mass binary made a close pass to the Sun in the past 100 kyr.
Carl Melis - One of the best experts on this subject based on the ideXlab platform.
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radio emission and Orbital Motion from the close encounter star brown dwarf binary wise j072003 20 084651 2
The Astronomical Journal, 2015Co-Authors: Adam J Burgasser, Carl Melis, Jacob Todd, Christopher R Gelino, Gregg Hallinan, Daniella Bardalez C GagliuffiAbstract:We report the detection of radio emission and Orbital Motion from the nearby star–brown dwarf binary WISE J072003.20–084651.2AB. Radio observations across the 4.5–6.5 GHz band with the Very Large Array identify at the position of the system quiescent emission with a flux density of 15 ± 3 μJy, and a highly polarized radio source that underwent a 2–3 minute burst with peak flux density 300 ± 90 μJy. The latter emission is likely a low-level magnetic flare similar to optical flares previously observed for this source. No outbursts were detected in separate narrow-band Hα monitoring observations. We report new high-resolution imaging and spectroscopic observations that confirm the presence of a co-moving T5.5 secondary and provide the first indications of three-dimensional Orbital Motion. We used these data to revise our estimates for the Orbital period (4.1_(-1.3)^(+2.7) year) and tightly constrain the Orbital inclination to be nearly edge-on (93o6^(+1o6)_(−1o4)), although robust measures of the component and system masses will require further monitoring. The inferred Orbital Motion does not change the high likelihood that this radio-emitting very low-mass binary made a close pass to the Sun in the past 100 kyr.
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radio emission and Orbital Motion from the close encounter star brown dwarf binary wise j072003 20 084651 2
arXiv: Solar and Stellar Astrophysics, 2015Co-Authors: Adam J Burgasser, Carl Melis, Jacob Todd, Christopher R Gelino, Gregg Hallinan, Daniella Bardalez C GagliuffiAbstract:We report the detection of radio emission and Orbital Motion from the nearby star-brown dwarf binary WISE J072003.20-084651.2AB. Radio observations across the 4.5-6.5 GHz band with the Very Large Array identify at the position of the system quiescent emission with a flux density of 15$\pm$3 $\mu$Jy, and a highly-polarized radio source that underwent a 2-3 min burst with peak flux density 300$\pm$90 $\mu$Jy. The latter emission is likely a low-level magnetic flare similar to optical flares previously observed for this source. No outbursts were detected in separate narrow-band H$\alpha$ monitoring observations. We report new high-resolution imaging and spectroscopic observations that confirm the presence of a co-moving T5.5 secondary and provide the first indications of three-dimensional Orbital Motion. We used these data to revise our estimates for the Orbital period (4.1$^{+2.7}_{-1.3}$ yr) and tightly constrain the Orbital inclination to be nearly edge-on (93.6\deg$^{+1.6\deg}_{-1.4\deg}$), although robust measures of the component and system masses will require further monitoring. The inferred Orbital Motion does not change the high likelihood that this radio-emitting very low-mass binary made a close pass to the Sun in the past 100 kyr.
Gregg Hallinan - One of the best experts on this subject based on the ideXlab platform.
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radio emission and Orbital Motion from the close encounter star brown dwarf binary wise j072003 20 084651 2
The Astronomical Journal, 2015Co-Authors: Adam J Burgasser, Carl Melis, Jacob Todd, Christopher R Gelino, Gregg Hallinan, Daniella Bardalez C GagliuffiAbstract:We report the detection of radio emission and Orbital Motion from the nearby star–brown dwarf binary WISE J072003.20–084651.2AB. Radio observations across the 4.5–6.5 GHz band with the Very Large Array identify at the position of the system quiescent emission with a flux density of 15 ± 3 μJy, and a highly polarized radio source that underwent a 2–3 minute burst with peak flux density 300 ± 90 μJy. The latter emission is likely a low-level magnetic flare similar to optical flares previously observed for this source. No outbursts were detected in separate narrow-band Hα monitoring observations. We report new high-resolution imaging and spectroscopic observations that confirm the presence of a co-moving T5.5 secondary and provide the first indications of three-dimensional Orbital Motion. We used these data to revise our estimates for the Orbital period (4.1_(-1.3)^(+2.7) year) and tightly constrain the Orbital inclination to be nearly edge-on (93o6^(+1o6)_(−1o4)), although robust measures of the component and system masses will require further monitoring. The inferred Orbital Motion does not change the high likelihood that this radio-emitting very low-mass binary made a close pass to the Sun in the past 100 kyr.
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radio emission and Orbital Motion from the close encounter star brown dwarf binary wise j072003 20 084651 2
arXiv: Solar and Stellar Astrophysics, 2015Co-Authors: Adam J Burgasser, Carl Melis, Jacob Todd, Christopher R Gelino, Gregg Hallinan, Daniella Bardalez C GagliuffiAbstract:We report the detection of radio emission and Orbital Motion from the nearby star-brown dwarf binary WISE J072003.20-084651.2AB. Radio observations across the 4.5-6.5 GHz band with the Very Large Array identify at the position of the system quiescent emission with a flux density of 15$\pm$3 $\mu$Jy, and a highly-polarized radio source that underwent a 2-3 min burst with peak flux density 300$\pm$90 $\mu$Jy. The latter emission is likely a low-level magnetic flare similar to optical flares previously observed for this source. No outbursts were detected in separate narrow-band H$\alpha$ monitoring observations. We report new high-resolution imaging and spectroscopic observations that confirm the presence of a co-moving T5.5 secondary and provide the first indications of three-dimensional Orbital Motion. We used these data to revise our estimates for the Orbital period (4.1$^{+2.7}_{-1.3}$ yr) and tightly constrain the Orbital inclination to be nearly edge-on (93.6\deg$^{+1.6\deg}_{-1.4\deg}$), although robust measures of the component and system masses will require further monitoring. The inferred Orbital Motion does not change the high likelihood that this radio-emitting very low-mass binary made a close pass to the Sun in the past 100 kyr.
