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We performed follow-up photometric observations on exoplanetary system HAT-P-37 from 2011 February to 2019 September. The nine new transit light curves of the R and V bands are presented in this work. Based on the new light curves and published literature data, the physical and orbital parameters of HAT-P-37 are refined. In addition, mid-transit times are obtained to update the linear ephemeris, Tc[0] = 2456478.57916 ± 0.00077 [BJDTDB], P = 2.7974415 ± 0.0000025 d. Moreover, the transit timing variations (TTVs) have an rms of 57 s and there is no significant TTV signal. According to dynamic analysis, we excluded the possibility of perturbers with a mass larger than 200M⊕, when located in 1 : 3, 1 : 2, 2 : 3 (interior) or 3 : 2, 2 : 1, 5 : 2, 3 : 1 (exterior) orbital resonance, respectively.

We present spectroscopic measurements of the Rossiter-McLaughlin effect for WASP-148b, the only known hot Jupiter with a nearby warm-Jupiter companion, from the WIYN/NEID and Keck/HIRES instruments. This is one of the first scientific results reported from the newly commissioned NEID spectrograph, as well as the second obliquity constraint for a hot Jupiter system with a close-in companion, after WASP-47. WASP-148b is consistent with being in alignment with the sky-projected spin axis of the host star, with $\lambda=-8^{\circ}.2^{{+8^{\circ}.7}}_{-9^{\circ}.7}$. The low obliquity observed in the WASP-148 system is consistent with the orderly-alignment configuration of most compact multi-planet systems around cool stars with obliquity constraints, including our solar system, and may point to an early history for these well-organized systems in which migration and accretion occurred in isolation, with relatively little disturbance. By contrast, previous results have indicated that high-mass and hot stars appear to more commonly host a wide range of misaligned planets: not only single hot Jupiters, but also compact systems with multiple super-Earths. We suggest that, to account for the high rate of spin-orbit misalignments in both compact multi-planet and isolated-hot-Jupiter systems orbiting high-mass and hot stars, spin-orbit misalignments may be caused by distant giant planet perturbers, which are most common around these stellar types., Comment: 13 pages, 4 figures, accepted for publication in ApJL

Convergent disk migration has long been suspected to be responsible for forming planetary systems with a chain of mean-motion resonances (MMR). Dynamical evolution over time could disrupt the delicate resonant configuration. We present TOI-1136, a 700-Myr-old G star hosting at least 6 transiting planets between $\sim$2 and 5 $R_\oplus$. The orbital period ratios deviate from exact commensurability by only $10^{-4}$, smaller than the $\sim$\,$10^{-2}$ deviations seen in typical Kepler near-resonant systems. A transit-timing analysis measured the masses of the planets (3-8$M_\oplus$) and demonstrated that the planets in TOI-1136 are in true resonances with librating resonant angles. Based on a Rossiter-McLaughlin measurement of planet d, the star's rotation appears to be aligned with the planetary orbital planes. The well-aligned planetary system and the lack of detected binary companion together suggest that TOI-1136's resonant chain formed in an isolated, quiescent disk with no stellar fly-by, disk warp, or significant axial asymmetry. With period ratios near 3:2, 2:1, 3:2, 7:5, and 3:2, TOI-1136 is the first known resonant chain involving a second-order MMR (7:5) between two first-order MMR. The formation of the delicate 7:5 resonance places strong constraints on the system's migration history. Short-scale (starting from $\sim$0.1 AU) Type-I migration with an inner disk edge is most consistent with the formation of TOI-1136. A low disk surface density ($\Sigma_{\rm 1AU}\lesssim10^3$g~cm$^{-2}$; lower than the minimum-mass solar nebula) and the resultant slower migration rate likely facilitated the formation of the 7:5 second-order MMR. TOI-1136's deep resonance suggests that it has not undergone much resonant repulsion during its 700-Myr lifetime. One can rule out rapid tidal dissipation within a rocky planet b or obliquity tides within the largest planets d and f., Comment: 48 pages, 23 figures, 8 tables. Accepted to AAS journals. Comments welcome!

The distribution of spin-orbit angles for systems with wide-separation, tidally detached exoplanets offers a unique constraint on the prevalence of dynamically violent planetary evolution histories. Tidally detached planets provide a relatively unbiased view of the primordial stellar obliquity distribution, since they cannot tidally realign within the system lifetime. We present the third result from our Stellar Obliquities in Long-period Exoplanet Systems (SOLES) survey: a measurement of the Rossiter-McLaughlin effect across two transits of the tidally detached warm Jupiter TOI-1478 b with the WIYN/NEID and Keck/HIRES spectrographs, revealing a sky-projected spin-orbit angle $\lambda=6.2^{+5.9}_{-5.5}$ degrees. Combining this new measurement with the full set of archival obliquity measurements, including two previous constraints from the SOLES survey, we demonstrate that, in single-star systems, tidally detached warm Jupiters are preferentially more aligned than closer-orbiting hot Jupiters. This finding has two key implications: (1) planets in single-star systems tend to form within aligned protoplanetary disks, and (2) warm Jupiters form more quiescently than hot Jupiters, which, in single-star systems, are likely perturbed into a misaligned state through planet-planet interactions in the post-disk-dispersal phase. We also find that lower-mass Saturns span a wide range of spin-orbit angles, suggesting a prevalence of planet-planet scattering and/or secular mechanisms in these systems., Comment: Accepted for publication in AJ. 20 pages, 7 figures, 4 tables

The fraction of observable nights is an essential parameter for selecting astronomical sites. In recent years, meteorological satellite data have played an essential role in recognising and providing statistics of observable nights. We present a method to estimate the fraction of observable nights based on the FengYun-2 series of geostationary meteorological satellites and weather records of multiple astronomical sites. We have calculated the fraction of observable nights at 27 sites in Indonesia and two astronomical sites in China to validate the method. The results derived from our method show good agreement with previous works. Furthermore, we have derived the yearly distribution of the fraction of observable nights above China, which indicates the area near 40$^{\circ}$N has more observable nights than other areas in China., Comment: 9 pages, 5 figures; accepted for publication in MNRAS (Acceptation date: 2022 February 10)

Obliquity measurements for stars hosting relatively long-period giant planets with weak star-planet tidal interactions may play a key role in distinguishing between formation theories for shorter-period hot Jupiters. Few such obliquity measurements have been made to date due to the relatively small sample of known wide-orbiting, transiting Jovian-mass planets and the challenging nature of these targets, which tend to have long transit durations and orbit faint stars. We report a measurement of the Rossiter–McLaughlin effect across the transit of K2-140 b, a Jupiter-mass planet with period P = 6.57 days orbiting a V = 12.6 star. We find that K2-140 is an aligned system with projected spin–orbit angle λ = 0.5° ± 9.7°, suggesting a dynamically cool formation history. This observation builds toward a population of tidally detached giant planet spin–orbit angles that will enable a direct comparison with the distribution of close-orbiting hot-Jupiter orbital configurations, elucidating the prevalent formation mechanisms of each group.

Radar signal-based object detection has become a primary and critical issue for autonomous driving recently. Recently advanced radar object detectors indicated that the cross-model supervision-based approach presented a promising performance based on 3D hourglass convolutional networks. However, the trade-off between computational efficiency and performance of radar object detection tasks is rarely investigated. When higher performance is required in the detection tasks, the 3D convolutional backbone network rarely meets the real-time applications. This paper proposes a lightweight, computationally efficient, and effective network architecture to conquer this issue. First, Atrous convolution, as well-known as dilated convolution, is adopted in our backbone network to make a smaller convolutional kernel having a larger receptive field so as a larger convolutional kernel can be eliminated to reduce the number of parameters. Furthermore, a densely connected residual block (DCSB) is proposed to better deliver the gradient flow from the loss function to improve the feature representation ability. Finally, the hourglass network structure is made by stacking several DCSBs with Mish activation function to form our detection network, termed as DCSN. In this manner, we can keep a larger receptive field and reduce the number of parameters significantly, resulting in an efficient radar object detector. Experiments are demonstrated that the proposed DCSN achieves a significant improvement of inference time and computational complexity, with comparable performance for radar object detection. The source code can be found in https://github.com/jesse1029/RADER-DCSN.

Measuring the obliquity distribution of stars hosting warm Jupiters may help us to understand the formation of close-orbiting gas giants. Few such measurements have been performed due to practical difficulties in scheduling observations of the relatively infrequent and long-duration transits of warm Jupiters. Here, we report a measurement of the Rossiter-McLaughlin effect for K2-232b, a warm Jupiter (M_P=0.39 M_Jup) on an 11.17-day orbit with an eccentricity of 0.26. The data were obtained with the Automated Planet Finder during two separate transits. The planet's orbit appears to be well-aligned with the spin axis of the host star, with a projected spin-orbit angle of lambda = -11.1+/-6.6 deg. Combined with the other available data, we find that high obliquities are almost exclusively associated with planets that either have an orbital separation greater than 10 stellar radii or orbit stars with effective temperatures hotter than 6,000K. This pattern suggests that the obliquities of the closest-orbiting giant planets around cooler stars have been damped by tidal effects., Comment: Accepted for publication in AJ, 8 Pages, 4 Figures

We report the discovery and confirmation of two new hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS): TOI 564 b and TOI 905 b. The transits of these two planets were initially observed by TESS with orbital periods of 1.651 d and 3.739 d, respectively. We conducted follow-up observations of each system from the ground, including photometry in multiple filters, speckle interferometry, and radial velocity measurements. For TOI 564 b, our global fitting revealed a classical hot Jupiter with a mass of $1.463^{+0.10}_{-0.096}\ M_J$ and a radius of $1.02^{+0.71}_{-0.29}\ R_J$. TOI 905 b is a classical hot Jupiter as well, with a mass of $0.667^{+0.042}_{-0.041}\ M_J$ and radius of $1.171^{+0.053}_{-0.051}\ R_J$. Both planets orbit Sun-like, moderately bright, mid-G dwarf stars with V ~ 11. While TOI 905 b fully transits its star, we found that TOI 564 b has a very high transit impact parameter of $0.994^{+0.083}_{-0.049}$, making it one of only ~20 known systems to exhibit a grazing transit and one of the brightest host stars among them. TOI 564 b is therefore one of the most attractive systems to search for additional non-transiting, smaller planets by exploiting the sensitivity of grazing transits to small changes in inclination and transit duration over the time scale of several years., 21 pages and 10 figures. Submitted to AJ

We present 127 new transit light curves for 39 hot Jupiter systems, obtained over the span of five years by two ground-based telescopes. A homogeneous analysis of these newly collected light curves together with archived spectroscopic, photometric, and Doppler velocimetric data using EXOFASTv2 leads to a significant improvement in the physical and orbital parameters of each system. All of our stellar radii are constrained to accuracies of better than 3\%. The planetary radii for 37 of our 39 targets are determined to accuracies of better than $5\%$. Compared to our results, the literature eccentricities are preferentially overestimated due to the Lucy-Sweeney bias. Our new photometric observations therefore allow for significant improvement in the orbital ephemerides of each system. Our correction of the future transit window amounts to a change exceeding $10\,{\rm min}$ for ten targets at the time of JWST's launch, including a $72\,{\rm min}$ change for WASP-56. The measured transit mid-times for both literature light curves and our new photometry show no significant deviations from the updated linear ephemerides, ruling out in each system the presence of companion planets with masses greater than $0.39 - 5.0\, rm M_{\oplus}$, $1.23 - 14.36\, \rm M_{\oplus}$, $1.65 - 21.18\, \rm M_{\oplus}$, and $0.69 - 6.75\, \rm M_{\oplus}$ near the 1:2, 2:3, 3:2, and 2:1 resonances with the hot Jupiters , respectively, at a confidence level of $\pm 1\,\sigma$. The absence of resonant companion planets in the hot Jupiter systems is inconsistent with the conventional expectation from disk migration., Comment: 28 pages,9 figures, accepted for publication in ApJS

Objective: To investigate the effect of dexmedetomidine combined with parecoxib sodium on the levels of inflammatory factors, blood gas analysis and stress hormone in patients undergoing radical resection of esophageal carcinoma during one lung ventilation. Methods: According to the random data table, 81 cases of esophageal cancer patients were divided into the control group (n=41) and observation group (n=40), the patients in the two groups underwent left thoracotomy esophageal cancer radical resection, the control group patients were treated with parecoxib sodium, and patients in the observation group were treated with parecoxib sodium combined with dexmedetomidine medetomidine treatment, before induction of anesthesia (T 0 ), 30 min of one lung ventilation (T 1 ) and 120 min after operation (T 2 ) at three time points, the levels of inflammatory factors [tumor necrosis factor-α (TNF-α), C reactive protein (CRP)], blood gas analysis[oxygen partial pressure (PaO 2 ), carbon dioxide partial pressure (PaCO 2 )] and stress hormone[epinephrine (E), norepinephrine (NE)] of the two groups were compared. Results: Intra group level comparison, compared with the levels of two groups at the T 0 moment, the levels of TNF-α, CRPand NE of theT 1 and T 2 moment were significantly increased, the level of PaO 2 were significantly decreased, and T 2 moment levels were significantly higher than that of T 1 moment, the difference was statistical significance; There were no significant differences between the two groups of the levels of TNF-α, CRP, PaO 2 , E and NE of the T 0 moment, the levels of TNF-α, CRP, E and NE of the observation group at the T 1 and T 2 moment were significantly lower than the control group, at the same time the PaO 2 level was significantly higher than the control group, the difference was statistically significant; There were no statistically significant differences in PaCO 2 levels between groups and at any time. Conclusion: Dexmedetomidine combined with parecoxib sodium can effectively relieve the inflammatory stress, improve the levels of the blood gas analysis index and stress hormone during one lung ventilation, has an important clinical value.

We report the first confirmation of a hot Jupiter discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HD 202772A b. The transit signal was detected in the data from TESS Sector 1, and was confirmed to be of planetary origin through radial-velocity measurements. HD 202772A b is orbiting a mildly evolved star with a period of 3.3 days. With an apparent magnitude of V = 8.3, the star is among the brightest known to host a hot Jupiter. Based on the 27days of TESS photometry, and radial velocity data from the CHIRON and HARPS spectrographs, the planet has a mass of 1.008+/-0.074 M_J and radius of 1.562+/-0.053 R_J , making it an inflated gas giant. HD 202772A b is a rare example of a transiting hot Jupiter around a quickly evolving star. It is also one of the most strongly irradiated hot Jupiters currently known., Comment: Submitted to AAS Journal

We present ten $R$-band photometric observations of eight different transits of the hot Jupiter HAT-P-33b, which has been targeted by our Transiting Exoplanet Monitoring Project (TEMP). The data were obtained by two telescopes at the Xinglong Station of National Astronomical Observatories of China (NAOC) from 2013 December through 2016 January, and exhibit photometric scatter of $1.6-3.0\,\rm{mmag}$. After jointly analyzing the previously published photometric data, radial-velocity (RV) measurements, and our new light curves, we revisit the system parameters and orbital ephemeris for the HAT-P-33b system. Our results are consistent with the published values except for the planet-to-star radius ratio ($R_{P}/R_{*}$), the ingress/egress duration ($\tau$) and the total duration ($T_{14}$), which together indicate a slightly shallower and shorter transit shape. Our results are based on more complete light curves, whereas the previously published work had only one complete transit light curve. No significant anomalies in Transit Timing Variations (TTVs) are found, and we place upper mass limits on potential perturbers, largely supplanting the loose constraints provided by the extant RV data. The TTV limits are stronger near mean-motion resonances, especially for the low-order commensurabilities. We can exclude the existence of a perturber with mass larger than 0.6, 0.3, 0.5, 0.5, and $0.3\,{\rm M_\oplus}$ near the 1:3, 1:2, 2:3, 3:2, and 2:1 resonances, respectively., Comment: Accepted for AJ

In the two stage supply chain with one manufacturer and one retailer, the double sided moral hazard is considered as the sales influenced by both the manufacturer’s and the retailer’s effort. In theory, the quantity discount contract can motive the manufacturer and the retailer to put the optimal effort, and make the supply chain get the most earning, which can be divided arbitrarily. In experiment, the effort of the retailer and order quantity are influenced by the ratio of the earning divided, but the effort of the manufacturer is not sufficient, hardly influenced by the ratio of the ratio divided. Unlike the theory, the quantity discount contract can not make the supply chain’s earning optimal. The analysis of the causes of the manufacturer’s insufficient investment in three aspects, risk attitude, characteristics of the input and the allocation of decision rights, is given to provide guidance for the practice of the supply chain with double moral hazard.

LX Ser is a deeply eclipsing cataclysmic variable with an orbital period of $0.^d 1584325$. Sixty two new eclipse times were determined by our observations and the AAVSO International Data base. Combining all available eclipse times, we analyzed the O-C behavior of LX Ser. We found that the O-C diagram of LX Ser shows a sinusoidal oscillation with a period of 22.8 yr and an amplitude of 0.00035 days. Two mechanisms (i.e., the Applegate mechanism and the light travel time effect) are applied to explain the cyclic modulation. We found that the Applegate mechanism is difficult to explain the cyclic oscillation in the orbital period. Therefore, the cyclic period change is most likely to be caused by the light travel time effect due to the presence of a third body. The mass of the tertiary component was determined to be $M_3\sim7.5 M_{Jup}$. We supposed that the tertiary companion is plausible a giant planet. The stability of the giant planet was checked, and we found that the multiple system is stable., Comment: Submitted to PASJ, 20 pages, 7 figures

Although EMD can implement adaptive separation between leak signal and strong background noise, the IMFs used for leak signal reconstruction always change with the varying frequency components. In this paper, an evaluation criteria for leak signal is defined and a method based on the analysis result of EMD for adaptive reconstruction is presented. The results of signal reconstruction and identifying leak location based on field test show this method is feasible and reliable.

We present eight new light curves of the transiting extra-solar planet HAT-P-25b obtained from 2013 to 2016 with three telescopes at two observatories. We use the new light curves, along with recent literature material, to estimate the physical and orbital parameters of the transiting planet. Specifically, we determine the mid-transit times (T$_{C}$) and update the linear ephemeris, T$_{C[0]}$=2456418.80996$\pm$0.00025 [$\mathrm{BJD}_\mathrm{TDB}$] and P=3.65281572$\pm$0.00000095 days. We carry out a search for transit timing variations (TTVs), and find no significant TTV signal at the $\Delta T=$80 s-level, placing a limit on the possible strength of planet-planet interactions ($\mathrm{TTV_{G}}$). In the course of our analysis, we calculate the upper mass-limits of the potential nearby perturbers. Near the 1:2, 2:1, and 3:1 resonances with HAT-P-25b, perturbers with masses greater than 0.5, 0.3, and 0.5 $\mathrm{M_{\oplus}}$ respectively, can be excluded. Furthermore, based on the analysis of TTVs caused by light travel time effect (LTTE) we also eliminate the possibility that a long-period perturber exists with $M_{\rm p}> 3000 \,\mathrm{M_{J}}$ within $a=11.2\,{\rm AU}$ of the parent star., Comment: Published in PASP

In many cases, IPR holders of technologies have control rights in negotiation while they should take consideration of reasonable requests from partners. If customers have difficulty in quality identification, how to design the cooperation contracts influenced by both adverse selection problem and moral hazard problem for multi-agent technology-transformation projects? The results show us that negative effect relating to partners' high effort and security benefits promised to partners will influence the final designing result.

Information asymmetry widely exists in the supply chain. The supply chain cannot be coordinated easily because of it. But coordination is important to maximize the profit of supply chain. In this paper, the situation that supplier has adverse selection and the retailer has moral hazard for information asymmetry is considered. A virtual third party is introduced to develop an incentive model from the perspective of supply chain. The result shows that this method can coordinate the supply chain under information asymmetry. And the model is proved to be the same as that in real world.

With the increasing of market competition, human dispatching service can reduce enterprise's human resources cost. But asymmetric information among principal, dispatching agency and dispatched workers may cause moral hazard of dispatching agency and dispatched workers. This paper considers moral hazard under asymmetric information. It researches the maximum problem of principal's profit under the incentive compatibility constraints of considering dispatching agency and dispatched workers. Through model analysis it commissioned that principal can adjust the incentive coefficient in order to better motivate dispatching agency and dispatched workers, so that the requester to obtain more revenue.

To observe the analgesic effect of intrathecal transplant of immortalized rat astrocyte genetically modified by human preproenkephalin gene (IAST/hPPE) on chronic neuropathic pain.40 adult male Sprague-Dawley rats were randomly divided into four groups, 10 rats for each group. Naive group, SNI group, SNI + IAST group and SNI + IAST/hPPE group. The immortalized rat astrocyte (IAST) or IAST/hPPE co-incubated with bromodeoxyuridine (BrdU) in vitro were transplanted in the lumbar 4 to 6 subarachnoid space near the spinal cord 1 week after right side spared nerve injury (SNI). All animals were tested for bilateral 50% hindpaw withdrawal threshold (PWT) to a graded series of Von Frey hairs stimulation once a week from one week before SNI to six weeks after transplant, the difference value for right 50% PWT minus left 50% PWT was calculated and the effect of intraperitoneal naloxone on the analgesic efficacies was also observed. The content of L-EK in the spinal cord of L4 - 6 and was determined using immunohistochemistry and radioimmunoassay, and the expression of BrdU in grafts was determined using immunohistochemistry.Allodynia-like behaviour after 1 week following SNI was observed. As compared with Naive group, the difference value for the right 50% PWT minus left 50% PWT in the other three groups was higher significantly (P0.01). The tactile allodynia induced by SNI was significantly alleviated during the 1 to 6 week period after transplantation of IAST/hPPE cells, but transplants of IAST cells had no effect on the allodynia-like behaviour. The difference value for the right 50% PWT minus left 50% PWT in SNI + IAST/hPPE group was lower significantly than that in the SNI and SNI +I AST group (P0.01), but there was no significant difference between SNI and SNI + IAST group (P0.05). The efficacies were reversed by intraperitoneal naloxone in SNI + IAST/hPPE group. The content of L-EK in the lumbar spinal cord in IAST/hPPE group (108.1 pg/mg +/- 12.5 pg/mg) was significantly higher than that in other three groups (P0.01), but there was no significant difference between SNI and SNI + IAST group (25.4 pg/mg +/- 1.9 pg/mg vs 28.0 pg/mg +/- 2.1 pg/mg, P0.05). Furthermore, The grafts in the surface of dorsal horn were still stained positively for BrdU, they survived greater than 6 weeks on the pia mater around the spinal cord.Intrathecal transplant of IAST/hPPE cells could alleviate the allodynia-like behaviour after chronic neuropathic pain, which is associated with enkephalin secreted continuously from the grafts and conducted via opiate receptors.