Machine Learning Based Real Bogus System for HSC-SSP Moving Object Detecting Pipeline [IMA]

http://arxiv.org/abs/1704.06413


The machine learning techniques are widely applied in many modern optical sky surveys, i.e. Pan-STARRS1, PTF/iPTF and Subaru/Hyper Suprime-Cam survey, to reduce the human intervention for data verification. In this study, we have established a machine learning based real-bogus system to reject the false detections in the HSC-SSP source catalog. Therefore the HSC-SSP moving object detection pipeline can operate more effectively due to the much less false positives inputs. To train the real-bogus system, we use the stationary sources as the real training set and the `flagged’ data as the bogus set. The training set contains 49 features, which, in majority, are the photometry measurements and shape moments generating from the HSC image reduction pipeline (hscPipe). Our system can reach a true positive rate (tpr) ~ 96% with a false positive rate (fpr) ~ 1% or tpr ~ 99% at fpr ~ 5%. Therefore we conclude that the stationary sources are decent real training samples, and using photometry measurements and shape moments can reject the false positives effectively.

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H. Lin, Y. Chen, J. Wang, et. al.
Mon, 24 Apr 17
3/54

Comments: 16 pages, 4 figures, submitted to PASJ HSC special issue

Constraints on the Magnetic Field Strength of HAT-P-7 b and other Hot Giant Exoplanets [EPA]

http://arxiv.org/abs/1704.06271


Observations of infrared and optical light curves of hot Jupiters have demonstrated that the peak brightness is generally offset eastward from the substellar point [1,2]. This observation is consistent with hydrodynamic numerical simulations that produce fast, eastward directed winds which advect the hottest point in the atmosphere eastward of the substellar point [3,4]. However, recent continuous Kepler measurements of HAT-P-7 b show that its peak brightness offset varies significantly in time, with excursions such that the brightest point is sometimes westward of the substellar point [5]. These variations in brightness offset require wind variability, with or without the presence of clouds. While such wind variability has not been seen in hydrodynamic simulations of hot Jupiter atmospheres, it has been seen in magnetohydrodynamic (MHD) simulations [6]. Here we show that MHD simulations of HAT-P-7 b indeed display variable winds and corresponding variability in the position of the hottest point in the atmosphere. Assuming the observed variability in HAT-P-7 b is due to magnetism we constrain its minimum magnetic field strength to be 6\,G. Similar observations of wind variability on hot giant exoplanets, or lack thereof, could help constrain their magnetic field strengths. Since dynamo simulations of these planets do not exist and theoretical scaling relations [7] may not apply, such observational constraints could prove immensely useful.

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T. Rogers
Mon, 24 Apr 17
15/54

Comments: 8 pages, 3 figures, Accepted at Nature Astronomy

Hydrodynamic ablation of protoplanetary disks via supernovae [SSA]

http://arxiv.org/abs/1704.06308


We present three-dimensional simulations of a protoplanetary disk subject to the effect of a nearby (0.3pc distant) supernova, using a time-dependent flow from a one dimensional numerical model of the supernova remnant (SNR), in addition to constant peak ram pressure simulations. Simulations are performed for a variety of disk masses and inclination angles. We find disk mass-loss rates that are typically 1e-7 to 1e-6 Msol/yr (but peak near 1e-5 Msol/yr during the “instantaneous” stripping phase) and are sustained for around 200 yr. Inclination angle has little effect on the mass loss unless the disk is close to edge-on. Inclined disks also strip asymmetrically with the trailing edge ablating more easily. Since the interaction lasts less than one outer rotation period, there is not enough time for the disk to restore its symmetry, leaving the disk asymmetrical after the flow has passed. Of the low-mass disks considered, only the edge-on disk is able to survive interaction with the SNR (with 50% of its initial mass remaining). At the end of the simulations, disks that survive contain fractional masses of SN material up to 5e-6. This is too low to explain the abundance of short-lived radionuclides in the early solar system, but a larger disk and the inclusion of radiative cooling might allow the disk to capture a higher fraction of SN material.

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J. Close and J. Pittard
Mon, 24 Apr 17
16/54

Comments: 16 pages, 16 figures, 2 tables, accepted by MNRAS

Spectra and physical properties of Taurid meteoroids [EPA]

http://arxiv.org/abs/1704.06482


Taurids are an extensive stream of particles produced by comet 2P/Encke, which can be observed mainly in October and November as a series of meteor showers rich in bright fireballs. Several near-Earth asteroids have also been linked with the meteoroid complex, and recently the orbits of two carbonaceous meteorites were proposed to be related to the stream, raising interesting questions about the origin of the complex and the composition of 2P/Encke. Our aim is to investigate the nature and diversity of Taurid meteoroids by studying their spectral, orbital, and physical properties determined from video meteor observations. Here we analyze 33 Taurid meteor spectra captured during the predicted outburst in November 2015 by stations in Slovakia and Chile, including 14 multi-station observations for which the orbital elements, material strength parameters, dynamic pressures, and mineralogical densities were determined. It was found that while orbits of the 2015 Taurids show similarities with several associated asteroids, the obtained spectral and physical characteristics point towards cometary origin with highly heterogeneous content. Observed spectra exhibited large dispersion of iron content and significant Na intensity in all cases. The determined material strengths are typically cometary in the $K_B$ classification, while $P_E$ criterion is on average close to values characteristic for carbonaceous bodies. The studied meteoroids were found to break up under low dynamic pressures of 0.02 – 0.10 MPa, and were characterized by low mineralogical densities of 1.3 – 2.5 g cm$^{-3}$. The widest spectral classification of Taurid meteors to date is presented.

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P. Matlovic, J. Toth, R. Rudawska, et. al.
Mon, 24 Apr 17
19/54

Comments: N/A

An Optical/near-infrared investigation of HD 100546 b with the Gemini Planet Imager and MagAO [EPA]

http://arxiv.org/abs/1704.06317


We present H band spectroscopic and Halpha photometric observations of HD 100546 obtained with GPI and MagAO. We detect H band emission at the location of the protoplanet HD 100546b, but show that choice of data processing parameters strongly affects the morphology of this source. It appears point-like in some aggressive reductions, but rejoins an extended disk structure in the majority of the others. Furthermore, we demonstrate that this emission appears stationary on a timescale of 4.6 yrs, inconsistent at the 2sigma level with a Keplerian clockwise orbit at 59 au in the disk plane. The H band spectrum of the emission is inconsistent with any type of low effective temperature object or accreting protoplanetary disk. It strongly suggests a scattered light origin, as it is consistent with the spectrum of the star and the spectra extracted at other locations in the disk. A non detection at the 5sigma level of HD 100546b in differential Halpha imaging places an upper limit, assuming the protoplanet lies in a gap free of extinction, on the accretion luminosity and accretion rate of 1.7E-4 Lsun and MMdot<6.4E-7Mjup^2/yr for 1Rjup. These limits are comparable to the accretion luminosity and rate of TTauri-stars or LkCa 15b. Taken together, these lines of evidence suggest that the H band source at the location of HD 100546b is not emitted by a planetary photosphere or an accreting circumplanetary disk but is a disk feature enhanced by the PSF subtraction process. This non-detection is consistent with the non-detection in the K band reported in an earlier study but does not exclude the possibility that HD 100546b is deeply embedded.

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J. Rameau, K. Follette, L. Pueyo, et. al.
Mon, 24 Apr 17
20/54

Comments: 10 pages, 5 figures, 1 table

The origin of the occurrence rate profile of gas giants inside 100 days [EPA]

http://arxiv.org/abs/1704.06383


We investigate the origin of the period distribution of giant planets. We try to fit the bias-corrected distribution of giant planets inside 300 days found by Santerne et al. (2016) using a planet formation model based on pebble accretion. We investigate two possible initial conditions: a linear distribution of planetary seeds, and seeds injected exclusively on the water and CO icelines. Our simulations exclude the linear initial distribution of seeds with a high degree of confidence. Our bimodal model based on snowlines give a more reasonable fit to the data, with the discrepancies reducing sig- nificantly if we assume the water snowline to be a factor 3-10 less efficient at producing planetary seeds. This model moreover performs better on both the warm/hot Jupiters ratio and the Gaussian mixture model as comparison criteria. Our results hint that the giant exoplanets population inside 300 days is more compatible with planets forming preferentially at special locations.

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M. Ali-Dib, A. Johansen and C. Huang
Mon, 24 Apr 17
25/54

Comments: 8 pages, 6 figures, submitted to MNRAS (revised version after the referee’s first report)

Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets [EPA]

http://arxiv.org/abs/1704.06459


We present an analytical and numerical study of the orbital migration and resonance capture of fictitious two-planet systems with masses in the super-Earth range undergoing Type-I migration. We find that, depending on the flare index and proximity to the central star, the average value of the period ratio, $P_2/P_1$, between both planets may show a significant deviation with respect to the nominal value. For planets trapped in the 2:1 commensurability, offsets may reach values on the order of $0.1$ for orbital periods on the order of $1$ day, while systems in the 3:2 mean-motion resonance (MMR) show much smaller offsets for all values of the semimajor axis. These properties are in good agreement with the observed distribution of near-resonant exoplanets, independent of their detection method. We show that 2:1-resonant systems far from the star, such as HD82943 and HR8799, are characterized by very small resonant offsets, while higher values are typical of systems discovered by Kepler with orbital periods approximately a few days. Conversely, planetary systems in the vicinity of the 3:2 MMR show little offset with no significant dependence on the orbital distance. In conclusion, our results indicate that the distribution of Kepler planetary systems around the 2:1 and 3:2 MMR are consistent with resonant configurations obtained as a consequence of a smooth migration in a laminar flared disk, and no external forces are required to induce the observed offset or its dependence with the commensurability or orbital distance from the star.

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X. Ramos, C. Charalambous, P. Benitez-Llambay, et. al.
Mon, 24 Apr 17
28/54

Comments: 11 pages, 7 figures, accepted for publication in A&A