The Experts below are selected from a list of 29508 Experts worldwide ranked by ideXlab platform
Larissa Nofi - One of the best experts on this subject based on the ideXlab platform.
-
simultaneous linear and circular optical polarimetry of asteroid 4 vesta
The Astrophysical Journal, 2015Co-Authors: Sloane Wiktorowicz, Larissa NofiAbstract:From a single 3.8 hr observation of the asteroid (4) Vesta at 137 phase angle with the POlarimeter at Lick for Inclination Studies of Hot jupiters 2 (POLISH2) at the Lick Observatory Shane 3 m telescope, we confirm rotational Modulation of linear polarization in the B and V bands. We measure the Peak-to-Peak Modulation in the degree of linear polarization to be ΔP = (294 ± 35) × 10−6 (ppm) and time-averaged ΔP/P = 0.0575 ± 0.0069. After rotating the plane of linear polarization to the scattering plane, asteroidal rotational Modulation is detected with 12σ confidence and observed solely in Stokes Q/I. POLISH2 simultaneously measures Stokes I, Q, U (linear polarization), and V (circular polarization), but we detect no significant circular polarization with a 1σ upper limit of 78 ppm in the B band. Circular polarization is expected to arise from multiple scattering of sunlight by rough surfaces, and it has previously been detected in nearly all other classes of solar system bodies except for asteroids. Subsequent observations may be compared with surface albedo maps from the Dawn Mission, which may allow the identification of compositional variation across the asteroidal surface. These results demonstrate the high accuracy achieved by POLISH2 at the Lick 3 m telescope, which is designed to directly detect scattered light from spatially unresolvable exoplanets.
-
simultaneous linear and circular optical polarimetry of asteroid 4 vesta
arXiv: Earth and Planetary Astrophysics, 2014Co-Authors: Sloane Wiktorowicz, Larissa NofiAbstract:From a single, 3.8-hour observation of asteroid (4) Vesta at $13.7^\circ$ phase angle with the POLISH2 polarimeter at the Lick Observatory Shane 3-m telescope, we confirm rotational Modulation of linear polarization in $B$ and $V$ bands. We measure the Peak-to-Peak Modulation in degree of linear polarization to be $\Delta P = (294 \pm 35) \times 10^{-6}$ (ppm) and time-averaged $\Delta P / P = 0.0577 \pm 0.0069$. After rotating the plane of linear polarization to the scattering plane, asteroidal rotational Modulation is detected with $12 \sigma$ confidence and observed solely in Stokes $Q/I$. POLISH2 simultaneously measures Stokes $I$, $Q$, $U$ (linear polarization), and $V$ (circular polarization), but we detect no significant circular polarization with a $1 \sigma$ upper limit of 140 ppm in $B$ band. Circular polarization is expected to arise from multiple scattering of sunlight by rough surfaces, and it has previously been detected in nearly all other classes of Solar System bodies save asteroids. Subsequent observations may be compared with surface albedo maps from the Dawn Mission, which may allow identification of compositional variation across the asteroidal surface. These results demonstrate the high accuracy achieved by POLISH2 at the Lick 3-m telescope, which is designed to directly detect scattered light from spatially unresolvable exoplanets.
S Zucker - One of the best experts on this subject based on the ideXlab platform.
-
kepler koi 13 01 detection of beaming and ellipsoidal Modulations pointing to a massive hot jupiter
Astronomy and Astrophysics, 2012Co-Authors: T Mazeh, Gil Nachmani, Gil Sokol, S Faigler, S ZuckerAbstract:KOI-13 was presented by the Kepler team as a candidate for having a giant planet — KOI-13.01, with orbital period of 1.7 d and transit depth of∼0.8%. We have analyzed the Kepler Q2 data of KOI-13, which was publicly available at the time of the submission of this paper, and derived the amplitudes of the beaming, ellipsoidal and reflection mo dulations — 8.6± 1.1, 66.8± 1.6 and 72.0± 1.5 ppm (parts per million), respectively. After the paper was submitted, Q3 data were released, so we repeated the analysis with the newly available light curve. The results of the two quarters were quite similar. From the amplitudes of the beaming and the ellipsoidal Modulations we derived two independent estimates of the mass of the secondary. Both estimates, 6± 3 MJup and 4± 2 MJup, suggested that KOI-13.01 was a massive planet, with one of the largest known radii. We also found in the data a periodicity of unknown origin with a period of 1.0595 d and a Peak-to-Peak Modulation of∼60 ppm. The light curve of Q3 revealed a few more small-amplitude periodicity with similar frequencies. It seemed as if the secondary occultation of KOI-13 was slightly deeper than the reflection Peakto-Peak Modulation by 16.8± 4.5 ppm. If real, this small difference was a measure of the thermal emission from the night side of KOI-13.01. We estimated the effective temperature to be 2600± 150 K, using a simplistic black-body emissivity approximation. We then derived the planetary geometrical and Bond albedos as a function of the day-side temperature. Our analysis suggested that the Bond albedo of KOI-13.01 might be substantially larger than the geometrical albedo.
-
kepler koi 13 01 detection of beaming and ellipsoidal Modulations pointing to a massive hot jupiter
arXiv: Earth and Planetary Astrophysics, 2011Co-Authors: T Mazeh, Gil Nachmani, Gil Sokol, S Faigler, S ZuckerAbstract:KOI-13 was presented by the Kepler team as a candidate for having a giant planet - KOI-13.01, with orbital period of 1.7 d and transit depth of ~0.8%. We have analyzed the Kepler Q2 data of KOI-13, which was publicly available at the time of the submission of this paper, and derived the amplitudes of the beaming, ellipsoidal and reflection Modulations: 8.6 +/- 1.1, 66.8 +/- 1.6 and 72.0 +/- 1.5 ppm (parts per million), respectively. After the paper was submitted, Q3 data were released, so we repeated the analysis with the newly available light curve. The results of the two quarters were quite similar. From the amplitude of the beaming Modulation we derived a mass of 10 +/- 2 M_Jup for the secondary, suggesting that KOI-13.01 was a massive planet, with one of the largest known radii. We also found in the data a periodicity of unknown origin with a period of 1.0595 d and a Peak-to-Peak Modulation of ~60 ppm. The light curve of Q3 revealed a few more small-amplitude periodicities with similar frequencies. It seemed as if the secondary occultation of KOI-13 was slightly deeper than the reflection Peak-to-Peak Modulation by 16.8 +/- 4.5 ppm. If real, this small difference was a measure of the thermal emission from the night side of KOI-13.01. We estimated the effective temperature to be 2600 +/- 150 K, using a simplistic black-body emissivity approximation. We then derived the planetary geometrical and Bond albedos as a function of the day-side temperature. Our analysis suggested that the Bond albedo of KOI-13.01 might be substantially larger than the geometrical albedo.
Sloane Wiktorowicz - One of the best experts on this subject based on the ideXlab platform.
-
simultaneous linear and circular optical polarimetry of asteroid 4 vesta
The Astrophysical Journal, 2015Co-Authors: Sloane Wiktorowicz, Larissa NofiAbstract:From a single 3.8 hr observation of the asteroid (4) Vesta at 137 phase angle with the POlarimeter at Lick for Inclination Studies of Hot jupiters 2 (POLISH2) at the Lick Observatory Shane 3 m telescope, we confirm rotational Modulation of linear polarization in the B and V bands. We measure the Peak-to-Peak Modulation in the degree of linear polarization to be ΔP = (294 ± 35) × 10−6 (ppm) and time-averaged ΔP/P = 0.0575 ± 0.0069. After rotating the plane of linear polarization to the scattering plane, asteroidal rotational Modulation is detected with 12σ confidence and observed solely in Stokes Q/I. POLISH2 simultaneously measures Stokes I, Q, U (linear polarization), and V (circular polarization), but we detect no significant circular polarization with a 1σ upper limit of 78 ppm in the B band. Circular polarization is expected to arise from multiple scattering of sunlight by rough surfaces, and it has previously been detected in nearly all other classes of solar system bodies except for asteroids. Subsequent observations may be compared with surface albedo maps from the Dawn Mission, which may allow the identification of compositional variation across the asteroidal surface. These results demonstrate the high accuracy achieved by POLISH2 at the Lick 3 m telescope, which is designed to directly detect scattered light from spatially unresolvable exoplanets.
-
simultaneous linear and circular optical polarimetry of asteroid 4 vesta
arXiv: Earth and Planetary Astrophysics, 2014Co-Authors: Sloane Wiktorowicz, Larissa NofiAbstract:From a single, 3.8-hour observation of asteroid (4) Vesta at $13.7^\circ$ phase angle with the POLISH2 polarimeter at the Lick Observatory Shane 3-m telescope, we confirm rotational Modulation of linear polarization in $B$ and $V$ bands. We measure the Peak-to-Peak Modulation in degree of linear polarization to be $\Delta P = (294 \pm 35) \times 10^{-6}$ (ppm) and time-averaged $\Delta P / P = 0.0577 \pm 0.0069$. After rotating the plane of linear polarization to the scattering plane, asteroidal rotational Modulation is detected with $12 \sigma$ confidence and observed solely in Stokes $Q/I$. POLISH2 simultaneously measures Stokes $I$, $Q$, $U$ (linear polarization), and $V$ (circular polarization), but we detect no significant circular polarization with a $1 \sigma$ upper limit of 140 ppm in $B$ band. Circular polarization is expected to arise from multiple scattering of sunlight by rough surfaces, and it has previously been detected in nearly all other classes of Solar System bodies save asteroids. Subsequent observations may be compared with surface albedo maps from the Dawn Mission, which may allow identification of compositional variation across the asteroidal surface. These results demonstrate the high accuracy achieved by POLISH2 at the Lick 3-m telescope, which is designed to directly detect scattered light from spatially unresolvable exoplanets.
T Mazeh - One of the best experts on this subject based on the ideXlab platform.
-
kepler koi 13 01 detection of beaming and ellipsoidal Modulations pointing to a massive hot jupiter
Astronomy and Astrophysics, 2012Co-Authors: T Mazeh, Gil Nachmani, Gil Sokol, S Faigler, S ZuckerAbstract:KOI-13 was presented by the Kepler team as a candidate for having a giant planet — KOI-13.01, with orbital period of 1.7 d and transit depth of∼0.8%. We have analyzed the Kepler Q2 data of KOI-13, which was publicly available at the time of the submission of this paper, and derived the amplitudes of the beaming, ellipsoidal and reflection mo dulations — 8.6± 1.1, 66.8± 1.6 and 72.0± 1.5 ppm (parts per million), respectively. After the paper was submitted, Q3 data were released, so we repeated the analysis with the newly available light curve. The results of the two quarters were quite similar. From the amplitudes of the beaming and the ellipsoidal Modulations we derived two independent estimates of the mass of the secondary. Both estimates, 6± 3 MJup and 4± 2 MJup, suggested that KOI-13.01 was a massive planet, with one of the largest known radii. We also found in the data a periodicity of unknown origin with a period of 1.0595 d and a Peak-to-Peak Modulation of∼60 ppm. The light curve of Q3 revealed a few more small-amplitude periodicity with similar frequencies. It seemed as if the secondary occultation of KOI-13 was slightly deeper than the reflection Peakto-Peak Modulation by 16.8± 4.5 ppm. If real, this small difference was a measure of the thermal emission from the night side of KOI-13.01. We estimated the effective temperature to be 2600± 150 K, using a simplistic black-body emissivity approximation. We then derived the planetary geometrical and Bond albedos as a function of the day-side temperature. Our analysis suggested that the Bond albedo of KOI-13.01 might be substantially larger than the geometrical albedo.
-
kepler koi 13 01 detection of beaming and ellipsoidal Modulations pointing to a massive hot jupiter
arXiv: Earth and Planetary Astrophysics, 2011Co-Authors: T Mazeh, Gil Nachmani, Gil Sokol, S Faigler, S ZuckerAbstract:KOI-13 was presented by the Kepler team as a candidate for having a giant planet - KOI-13.01, with orbital period of 1.7 d and transit depth of ~0.8%. We have analyzed the Kepler Q2 data of KOI-13, which was publicly available at the time of the submission of this paper, and derived the amplitudes of the beaming, ellipsoidal and reflection Modulations: 8.6 +/- 1.1, 66.8 +/- 1.6 and 72.0 +/- 1.5 ppm (parts per million), respectively. After the paper was submitted, Q3 data were released, so we repeated the analysis with the newly available light curve. The results of the two quarters were quite similar. From the amplitude of the beaming Modulation we derived a mass of 10 +/- 2 M_Jup for the secondary, suggesting that KOI-13.01 was a massive planet, with one of the largest known radii. We also found in the data a periodicity of unknown origin with a period of 1.0595 d and a Peak-to-Peak Modulation of ~60 ppm. The light curve of Q3 revealed a few more small-amplitude periodicities with similar frequencies. It seemed as if the secondary occultation of KOI-13 was slightly deeper than the reflection Peak-to-Peak Modulation by 16.8 +/- 4.5 ppm. If real, this small difference was a measure of the thermal emission from the night side of KOI-13.01. We estimated the effective temperature to be 2600 +/- 150 K, using a simplistic black-body emissivity approximation. We then derived the planetary geometrical and Bond albedos as a function of the day-side temperature. Our analysis suggested that the Bond albedo of KOI-13.01 might be substantially larger than the geometrical albedo.
S Faigler - One of the best experts on this subject based on the ideXlab platform.
-
kepler koi 13 01 detection of beaming and ellipsoidal Modulations pointing to a massive hot jupiter
Astronomy and Astrophysics, 2012Co-Authors: T Mazeh, Gil Nachmani, Gil Sokol, S Faigler, S ZuckerAbstract:KOI-13 was presented by the Kepler team as a candidate for having a giant planet — KOI-13.01, with orbital period of 1.7 d and transit depth of∼0.8%. We have analyzed the Kepler Q2 data of KOI-13, which was publicly available at the time of the submission of this paper, and derived the amplitudes of the beaming, ellipsoidal and reflection mo dulations — 8.6± 1.1, 66.8± 1.6 and 72.0± 1.5 ppm (parts per million), respectively. After the paper was submitted, Q3 data were released, so we repeated the analysis with the newly available light curve. The results of the two quarters were quite similar. From the amplitudes of the beaming and the ellipsoidal Modulations we derived two independent estimates of the mass of the secondary. Both estimates, 6± 3 MJup and 4± 2 MJup, suggested that KOI-13.01 was a massive planet, with one of the largest known radii. We also found in the data a periodicity of unknown origin with a period of 1.0595 d and a Peak-to-Peak Modulation of∼60 ppm. The light curve of Q3 revealed a few more small-amplitude periodicity with similar frequencies. It seemed as if the secondary occultation of KOI-13 was slightly deeper than the reflection Peakto-Peak Modulation by 16.8± 4.5 ppm. If real, this small difference was a measure of the thermal emission from the night side of KOI-13.01. We estimated the effective temperature to be 2600± 150 K, using a simplistic black-body emissivity approximation. We then derived the planetary geometrical and Bond albedos as a function of the day-side temperature. Our analysis suggested that the Bond albedo of KOI-13.01 might be substantially larger than the geometrical albedo.
-
kepler koi 13 01 detection of beaming and ellipsoidal Modulations pointing to a massive hot jupiter
arXiv: Earth and Planetary Astrophysics, 2011Co-Authors: T Mazeh, Gil Nachmani, Gil Sokol, S Faigler, S ZuckerAbstract:KOI-13 was presented by the Kepler team as a candidate for having a giant planet - KOI-13.01, with orbital period of 1.7 d and transit depth of ~0.8%. We have analyzed the Kepler Q2 data of KOI-13, which was publicly available at the time of the submission of this paper, and derived the amplitudes of the beaming, ellipsoidal and reflection Modulations: 8.6 +/- 1.1, 66.8 +/- 1.6 and 72.0 +/- 1.5 ppm (parts per million), respectively. After the paper was submitted, Q3 data were released, so we repeated the analysis with the newly available light curve. The results of the two quarters were quite similar. From the amplitude of the beaming Modulation we derived a mass of 10 +/- 2 M_Jup for the secondary, suggesting that KOI-13.01 was a massive planet, with one of the largest known radii. We also found in the data a periodicity of unknown origin with a period of 1.0595 d and a Peak-to-Peak Modulation of ~60 ppm. The light curve of Q3 revealed a few more small-amplitude periodicities with similar frequencies. It seemed as if the secondary occultation of KOI-13 was slightly deeper than the reflection Peak-to-Peak Modulation by 16.8 +/- 4.5 ppm. If real, this small difference was a measure of the thermal emission from the night side of KOI-13.01. We estimated the effective temperature to be 2600 +/- 150 K, using a simplistic black-body emissivity approximation. We then derived the planetary geometrical and Bond albedos as a function of the day-side temperature. Our analysis suggested that the Bond albedo of KOI-13.01 might be substantially larger than the geometrical albedo.