Gamma-Ray Orbital Modulation of the Transitioning Millisecond Pulsar Binary XSS J12270–4859

We report on gamma-ray orbital modulation of the transitioning MSP binary XSS J12270–4859 detected in the Fermi Large Area Telescope (LAT) data. We use long-term optical data taken with the XMM-Newton OM and the Swift UltraViolet Optical Telescope to inspect radio timing solutions that are limited to relatively short time intervals and find that extrapolation of the solutions aligns well with the phasing of the optical data over 15 yr. The Fermi-LAT data folded on the timing solutions exhibit significant modulation (p = 5 × 10−6) with a gamma-ray minimum at the inferior conjunction of the pulsar. Intriguingly, the source seems to show similar modulation in both the low-mass X-ray binary and the MSP states, implying that mechanisms for gamma-ray emission in the two states are similar. We discuss these findings and their implications using an intrabinary shock scenario.

Quest for the Upcoming Periastron Passage of an Episodic Dust Maker and Particle-accelerating Colliding-wind Binary: WR 125

We have carried out a long-term infrared and X-ray investigation of the colliding-wind binary WR 125 (WC7 + O9III). The source was monitored using AstroSat Soft X-ray Telescope and the Tata Institute of Fundamental Research Near Infrared Imaging Camera-II mounted at the back of 3.6 m Devasthal Optical Telescope. WR 125 appeared brighter in the near-infrared K-band during the years 2017–2021 which is attributed to another episode of dust formation similar to the one reported during the likely periastron passage at the beginning of the 1990s. This is further supported by enhanced emission observed in the W1 and W2 bands of Wide-field Infrared Survey Explorer from 2018–2019. By combining archival X-ray data sets with our new measurements, long-term variations have been noticed. The source reaches a lower emission state in 2020 June (close to the recent infrared maximum) which could be due to enhanced absorption of X-rays produced in the colliding-wind region by the WC stellar wind close to the periastron in an eccentric orbit. The time interval between the previous and latest X-ray low states may indicate an orbital period of 28–29 years, in fair agreement with the recurrence time of episodic dust production. We also discuss published radio measurements in the context of a common picture based on a long-period binary scenario. These results allow us to draw relevant guidelines for future multiwavelength observations of WR 125.

Magnetic Helicity Estimations in Models and Observations of the Solar Magnetic Field. IV. Application to Solar Observations

In this ISSI-supported series of studies on magnetic helicity in the Sun, we systematically implement different magnetic helicity calculation methods on high-quality solar magnetogram observations. We apply finite-volume, discrete flux tube (in particular, connectivity-based) and flux-integration methods to data from Hinode’s Solar Optical Telescope. The target is NOAA Active Region 10930 during a 1.5-day interval in 2006 December that included a major eruptive flare (SOL2006-12-13T02:14X3.4). Finite-volume and connectivity-based methods yield instantaneous budgets of the coronal magnetic helicity, while the flux-integration methods allow an estimate of the accumulated helicity injected through the photosphere. The objectives of our work are twofold: a cross-validation of methods, as well as an interpretation of the complex events leading to the eruption. To the first objective, we find (i) strong agreement among the finite-volume methods, (ii) a moderate agreement between the connectivity-based and finite-volume methods, (iii) an excellent agreement between the flux-integration methods, and (iv) an overall agreement between finite-volume- and flux-integration-based estimates regarding the predominant sign and magnitude of the helicity. To the second objective, we are confident that the photospheric helicity flux significantly contributed to the coronal helicity budget and that a right-handed structure erupted from a predominantly left-handed corona during the X-class flare. Overall, we find that the use of different methods to estimate the (accumulated) coronal helicity may be necessary in order to draw a complete picture of an active region corona, given the careful handling of identified data (preparation) issues, which otherwise would mislead the event analysis and interpretation.

Optical telescope with 3.75 ◦ field of view and pre-aperture slewing mirror with observation area of 50 ◦ ×120 ◦ for the system of observation of day time asteroids (the SODA project)

В работе предложена оптическая схема широкоугольного телескопа с полем зрения 3.75 ◦ и апертурой 30 см для космической системы обнаружения декаметровых астероидов (проект СОДА). Основная отличительная особенность телескопа - наличие предапертурного плоского зеркала, обеспечивающего область наведения 50 ◦ × 120 ◦ , время перенаведения между соседними площадками составит не более 3 с. Предложен современный КМОП детектор с мелким пикселем. В работе представлены области обзора телескопов проекта СОДА из точки Лагранжа L 1 при использовании двух, трех и четырех телескопов, кратко обсуждены преимущества и недостатки каждого из вариантов. We propose an optical scheme of a telescope with a field of view of 3.75 ◦ and 30 cm aperture for the space system for observation of decameter size asteroids (the SODA project). The main distinctive feature of this telescope is a pre-aperture flat mirror that provides an observation area of 50 ◦ ×120 ◦ and a repointing time between the adjacent fields of less than 3 s. A modern CMOS detector with a small pixel is proposed. Observable sky area when using 2, 3 and 4 telescopes are described. The advantages and disadvantages of each option are briefly discussed.

AUTOMATING THE ALERT RESPONSE OF THE NU TRANSIENT TELESCOPE AT ASSY-TURGEN ASTROPHYSICAL OBSERVATORY (NUTTELA-TAO)

Our project aims to identify the physical nature of gamma-ray burst (GRB) emission via measurement of the optical spectral shape of this emission during the prompt phase, usually lasting only 60 sec. These measurements require a fast-moving optical telescope and instrumentation to respond autonomously to real-time GRB alerts. The Nazarbayev University Transient Telescope at AssyTurgen Astrophysical Observatory (NUTTelA-TAO) has a 0.7 m aperture, and can point anywhere above the local horizon in 8 seconds. We receive GRB Alerts via internet socket connection to the Gamma Coordinates Network (GCN) at the telescope site. We measure the GRB prompt optical emission with the Burst Simultaneous Three-Channel Imager (BSTI), which incorporates 3 EMCCD cameras, at Sloan g', r', and i' bands, for simultaneous high time-resolution imaging as fast as a few hundred millisecond per frame. We describe our automated control system software, including the overall control algorithm, control of the telescope, control and actuation systems for the enclosure roof, control of the instrument, and inputs from weather and other sensors. The software system is based on the GNU data language (GDL) in a Linux environment, selected for ease of writing and de-bugging software, familiarity to the project scientists, and image analysis capabilities. We give system performance results obtained during the early commissioning period.

THE CHANGING EVENT SURVEY: TRANSIENTS, SPACE DEBRIS & NEOs

Motivated by the promising era of time-domain and multi-messenger astronomy, CHanging Event Survey (CHES) is designed to join the ongoing campaign with a powerful wide-field optical telescope array. CHES project aims to monitor the transient universe, including gamma-ray bursts, fast radio bursts, the electromagnetic counterpart of gravitational waves events (kilonova), supernova, variable stars, near-earth objects, and space debris. The array consists of 12 individual wide field refractors with aperture 280 mm, covering 600 square degrees in total. In the same project, two 800 mm prime focus telescopes can be triggered for follow-up observation. Furthermore, CHES can effectively monitor 300 square deg in a dual band simultaneously, which enable the array to do candidate identification and follow-up for the triggers from LIGO/Virgo collaboration, Fermi, Swift, GECam and SVOM satellites.

CHEOPS precision phase curve of the Super-Earth 55 Cancri e

Context. 55 Cnc e is a transiting super-Earth (radius 1.88 R⊕ and mass 8 M⊕) orbiting a G8V host star on a 17-h orbit. Spitzer observations of the planet’s phase curve at 4.5 μm revealed a time-varying occultation depth, and MOST optical observations are consistent with a time-varying phase curve amplitude and phase offset of maximum light. Both broadband and high-resolution spectroscopic analyses are consistent with either a high mean molecular weight atmosphere or no atmosphere for planet e. A long-term photometric monitoring campaign on an independent optical telescope is needed to probe the variability in this system. Aims. We seek to measure the phase variations of 55 Cnc e with a broadband optical filter with the 30 cm effective aperture space telescope CHEOPS and explore how the precision photometry narrows down the range of possible scenarios. Methods. We observed 55 Cnc for 1.6 orbital phases in March of 2020. We designed a phase curve detrending toolkit for CHEOPS photometry which allowed us to study the underlying flux variations in the 55 Cnc system. Results. We detected a phase variation with a full-amplitude of 72 ± 7 ppm, but did not detect a significant secondary eclipse of the planet. The shape of the phase variation resembles that of a piecewise-Lambertian; however, the non-detection of the planetary secondary eclipse, and the large amplitude of the variations exclude reflection from the planetary surface as a possible origin of the observed phase variations. They are also likely incompatible with magnetospheric interactions between the star and planet, but may imply that circumplanetary or circumstellar material modulate the flux of the system. Conclusions. This year, further precision photometry of 55 Cnc from CHEOPS will measure variations in the phase curve amplitude and shape over time.

Planetary Science in Ethiopia

<p>Planetary Science in Ethiopia research has been emerged in Ethiopia based on the establishment of Entoto Observatory and Research Center (EORC) as well as special commencement of special graduate in three specialized fields such as (astronomy and astrophysics, space science, remote sensing and Geodesy). The installation of the twining optical telescope and ratification of national space policy has opened many opportunities to focus of planetary science research and training in Ethiopia.  Ethiopia has progressed in research, training, and technology and infrastructure development in planetary science, space technology and astronomy. This paper will focus on planetary science and related activities, current development and future prospects.</p>