This symposium has highlighted key first steps made in addressing many goals of the IAU Strategic Plan for 2020–2030. Presentations on initiatives regarding education, with applications to development, outreach, equity, inclusion, big data, and heritage, are briefly summarized here. The many projects underway for the public, for students, for teachers, and for astronomers doing astronomy education research provide a foundation for future collaborative efforts, both regionally and globally.

For over 30 years, the MCE Sky Pedagogy Research Group (Italy) and Plaza del Cielo Complex (Argentina) had been offering teachers and educators many projects and activities related to training and teaching/learning processes having the sky and the study of the multiple relationships of humans with the sky as a focus of research. We have developed didactical methods based on direct experience, naked-eye activities, cooperation and exchange of experiences. The pandemic forced us to suspend the in-person meetings, which are at the center of our research in the Teaching of Astronomy, so we decided to react constructively exploring virtuality designing the course “Meet the skies of the world”. Two courses where developed from June to September 2020, each one having 4 virtual meetings of 2,5 hours each, with more than a hundred participants from different countries. A Level II course will be developed during the first semester of 2021.

Department of Astronomy, Kyoto University has been conducting astronomy outreach programs in Kyoto University Hospital since 2006. In this proceeding, we report our activities in the hospital, survey results from graduate students, and discuss future directions.

Astronomy in Armenia was popular since ancient times and Armenia is rich in its astronomical heritage, such as ancient and medieval Armenian calendars, records of astronomical events by ancient Armenians, the astronomical heritage of the Armenian medieval great thinker Anania Shirakatsi, etc. Armenian astronomical archives have accumulated vast number of photographic plates, films and other careers of observational data. The Digitized Markarian Survey or the First Byurakan Survey, is the most important low-dispersion spectroscopic database. It is one of the rare science items included in UNESCO “Memory of the World” Documentary Heritage list. The Byurakan Astrophysical Observatory (BAO) Plate Archive Project (2015–2021) will result in digitization and storage of some 37,000 astronomical plates and films and in creation of an Electronic Database for further research projects. Based on these data and archives and development of their interoperability, the Armenian Virtual Observatory was created and joined the International Virtual Observatory Alliance.

Over the past decade the free and open-source cross-platform desktop planetarium program Stellarium has gained not only most of the computational accuracy requirements for today’s amateur astronomers, but also unique capabilities for specialized applications in cultural astronomy research and astronomical outreach. A 3D rendering module can put virtual reconstructions of human-made monuments in their surrounding landscape under the day and night skies of their respective epochs, so that the user can investigate and experience the potential connection of architecture, landscape, light and shadow, and the sky. It also played a key role in an exhibition about Stonehenge in Austria.

Exchangeable “skycultures” allow the presentation of constellation patterns and mythological figures of non-Western cultures. Stellarium’s multi-language support allows community-driven translation of the whole program, which predestines its use in education also in minority languages.

Stellarium is developed by a very small core team, but is open to external contributions.

In this poster we present a study of the orientation of the church of San Adrián de Sasabé in Borau, Huesca (Spain) in a practical way. This church is a characteristic Romanesque construction, predominant in the High Middle Ages, mainly in southwestern Europe.

The apse of Romanesque churches are oriented towards the east. But, in some churches, the apse has three windows and these are oriented in the direction of the sunrises on the days of the solstices and equinoxes. But sunrises and sunsets depend on the latitude of the place.

The church of San Adrián de Sasabé, the object of our study, has three windows in the apse, which allows us to carry out the necessary calculations to determine its orientation with precision outside the church.

The report shows the current opportunities for obtaining astronomical knowledge in school and outside it, through the use of non-formal education. These are school and extracurricular activities, schools, astronomical competitions and Olympiads, observation expeditions. For 25 years Bulgaria has been participating in the International Olympiads in Astronomy and Astronomy and Astrophysics with National Teams. The role and place of the system of Public Astronomical Observatories and Planetaria in the system of non-formal education in astronomy are discussed (In Bulgaria there are 7 Public astronomical observatories with a planetarium). Specialized activities in their school forms allow the formation of sustainable astronomical knowledge and observational habits.

The dramatic nature and irregular frequency of solar eclipses may have helped trigger the development of human curiosity. If the kind of solar eclipses we experience on Earth are rare within the Universe, human-like curiosity may also be rare.

We review Big Data in Astronomy and its role in Astronomy Education. At present all-sky and large-area astronomical surveys and their catalogued data span over the whole range of electromagnetic spectrum, from gamma-ray to radio, as well as most important surveys giving optical images, proper motions, variability and spectroscopic data. Most important astronomical databases and archives are presented as well. They are powerful sources for many-sided efficient research using the Virtual Observatory (VO) environment. It is shown that using and analysis of Big Data accumulated in astronomy lead to many new discoveries. Using these data gives a significant advantage for Astronomy Education due to its attractiveness and due to big interest of young generation to computer science and technologies. The Computer Science itself benefits from data coming from the Universe and a new interdisciplinary science Astroinformatics has been created to manage these data.

TUIMP is an outreach and educational project providing astronomical booklets that can be folded from one single sheet of paper. The booklets are written by professional astronomers and are intended for a broad audience. They can be downloaded for free from www.tuimp.org and used in classrooms, planetariums and in astronomy festivals. Presently they are available in 11 languages. Participation for writing new booklets or translating in any language is very welcome.

Astronomy education and public outreach (EPO) is one of the important part of the future development of astronomy. During the past few years, as the rapid evolution of Internet and the continuous change of policy, the breeding environment of science EPO keep improving and the number of related projects show a booming trend. EPO is no longer just a matter of to teachers and science educators but also attracted the attention of professional astronomers. Among all activates of astronomy EPO, the data driven astronomy education and public outreach (abbreviated as DAEPO) is special and important. It benefits from the development of Big Data and Internet technology and is full of flexibility and diversity. We will present the history, definition, best practices and prospective development of DAEPO for better understanding this active field.

We present the results of the implementation of a didactic sequence based on the formulation and resolution of astronomical problems by seventh grade elementary school students from the Autonomous City of Buenos Aires, Argentina. Its objective is to generate a meaningful understanding of the heliocentric model of the Solar System from the systematization of topocentric observations of the sky, either direct or mediated by resources such as diagrams, Stellarium software and tables, which we correlate with the parallel globe, other models with specific material and the Solar System Scope software. Throughout the sequence we address topics such as the diurnal and annual movement of the Sun, the night sky, astronomical ephemeris, Moon phases and eclipses. These are developed in parallel to the sphericity of the Earth and the concept of motion in science. For each of these topics we start from its recognition. We then implement strategies to guide students towards a possible description from the local point of view, and then extend it to other locations on the surface of the Earth. We encourage them to explain their ideas about the possible links between these topocentric observations and the corresponding relative positions of the celestial objects as seen from an external point of view to the Earth. These ideas are then contrasted with geocentric and heliocentric models. Here we highlight the integrative instances in which the students formulated problems in small groups and shared them for their resolution. Thus, motivated and challenged by the collaboration between peers, they became the protagonists of their learning.

We have detected 27 new supernova remnants (SNRs) using a new data release of the GLEAM survey from the Murchison Widefield Array telescope, including the lowest surface brightness SNR ever detected, G 0.1 – 9.7. Our method uses spectral fitting to the radio continuum to derive spectral indices for 26/27 candidates, and our low-frequency observations probe a steeper spectrum population than previously discovered. None of the candidates have coincident WISE mid-IR emission, further showing that the emission is non-thermal. Using pulsar associations we derive physical properties for six candidate SNRs, finding G 0.1 – 9.7 may be younger than 10 kyr. Sixty per cent of the candidates subtend areas larger than 0.2 deg2 on the sky, compared to < 25% of previously detected SNRs. We also make the first detection of two SNRs in the Galactic longitude range 220°–240°.

This work makes available a further $2\,860~\text{deg}^2$ of the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey, covering half of the accessible galactic plane, across 20 frequency bands sampling 72–231 MHz, with resolution $4\,\text{arcmin}-2\,\text{arcmin}$. Unlike previous GLEAM data releases, we used multi-scale CLEAN to better deconvolve large-scale galactic structure. For the galactic longitude ranges $345^\circ < l < 67^\circ$, $180^\circ < l < 240^\circ$, we provide a compact source catalogue of 22 037 components selected from a 60-MHz bandwidth image centred at 200 MHz, with RMS noise $\approx10-20\,\text{mJy}\,\text{beam}^{-1}$ and position accuracy better than 2 arcsec. The catalogue has a completeness of 50% at ${\approx}120\,\text{mJy}$, and a reliability of 99.86%. It covers galactic latitudes $1^\circ\leq|b|\leq10^\circ$ towards the galactic centre and $|b|\leq10^\circ$ for other regions, and is available from Vizier; images covering $|b|\leq10^\circ$ for all longitudes are made available on the GLEAM Virtual Observatory (VO).server and SkyView.

We examined the latest data release from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey covering 345° < l < 60° and 180° < l < 240°, using these data and that of the Widefield Infrared Survey Explorer to follow up proposed candidate Supernova Remnant (SNR) from other sources. Of the 101 candidates proposed in the region, we are able to definitively confirm ten as SNRs, tentatively confirm two as SNRs, and reclassify five as H ii regions. A further two are detectable in our images but difficult to classify; the remaining 82 are undetectable in these data. We also investigated the 18 unclassified Multi-Array Galactic Plane Imaging Survey (MAGPIS) candidate SNRs, newly confirming three as SNRs, reclassifying two as H ii regions, and exploring the unusual spectra and morphology of two others.

The giant Hii region W 31 hosts the populous star cluster W 31-CL and others projected on or in the surroundings. The most intriguing object is the stellar cluster SGR 1806-20, which appears to be related to a Luminous Blue Variable (LBV)—a luminous supergiant star. We used the deep VVV J-, H-, and $K_S$-band photometry combined with 2MASS data in order to address the distance and other physical and structural properties of the clusters W 31-CL, BDS 113, and SGR 1806-20. Field-decontaminated photometry was used to analyse colour–magnitude diagrams (CMDs) and stellar radial density profiles, using procedures that our group has developed and employed in previous studies. We conclude that the clusters W 31-CL and BDS 113 are located at 4.5 and 4.8 kpc and have ages of 0.5 and 1 Myr, respectively. This result, together with the pre-main sequence distribution in the CMD, characterises them as members of the W 31 complex. The present photometry detects the stellar content, addressed in previous spectroscopic classifications, in the direction of the cluster SGR 1806-20, including the LBV, Wolf–Rayet, and foreground stars. We derive an age of $10\pm4\,\text{Myr}$ and a distance of $d_{\odot}=8.0\pm1.95\,\text{kpc}$ . The cluster is extremely absorbed, with $A_V=25\,\text{mag}$ . The present results indicate that SGR 1806-20 is more distant by a factor 1.8 with respect to the W 31 complex, and thus not physically related to it.

The Murchison Widefield Array (MWA) is an electronically steered low-frequency (<300 MHz) radio interferometer, with a ‘slew’ time less than 8 s. Low-frequency (∼100 MHz) radio telescopes are ideally suited for rapid response follow-up of transients due to their large field of view, the inverted spectrum of coherent emission, and the fact that the dispersion delay between a 1 GHz and 100 MHz pulse is on the order of 1–10 min for dispersion measures of 100–2000 pc/cm3. The MWA has previously been used to provide fast follow-up for transient events including gamma-ray bursts (GRBs), fast radio bursts (FRBs), and gravitational waves, using systems that respond to gamma-ray coordinates network packet-based notifications. We describe a system for automatically triggering MWA observations of such events, based on Virtual Observatory Event standard triggers, which is more flexible, capable, and accurate than previous systems. The system can respond to external multi-messenger triggers, which makes it well-suited to searching for prompt coherent radio emission from GRBs, the study of FRBs and gravitational waves, single pulse studies of pulsars, and rapid follow-up of high-energy superflares from flare stars. The new triggering system has the capability to trigger observations in both the regular correlator mode (limited to ≥0.5 s integrations) and using the Voltage Capture System (VCS, 0.1 ms integration) of the MWA and represents a new mode of operation for the MWA. The upgraded standard correlator triggering capability has been in use since MWA observing semester 2018B (July–Dec 2018), and the VCS and buffered mode triggers will become available for observing in a future semester.

Hα emission is one of the most prominent features of young stellar objects in the optical range, and importantly, the equivalent width (EW) of Hα emission [EW(Hα)] is used to characterise an evolutionary stage of young stars. The aim of this work is to identify and study the stellar objects with variable EW(Hα) in the young stellar cluster IC 348. We performed photometric and slit-less observations at several epochs in order to reveal the variable objects. Significant variability of EW(Hα) was found in 90 out of 127 examined stars. From all epochs of observations, 32 objects were classified as CTT (classical T Tauri) and 69 as WTT (weak-line T Tauri) objects. The fraction of the variables in these samples is ~60%. We also identified 20 stellar objects, which showed not only a significant variability of the EW, but which also change their apparent evolutionary stage (CTT ⇆ WTT). For six stars, Hα line was observed in both emission and absorption.

The analysis of data obtained over a wide wavelength range (from X-ray to mid-infrared) has shown that Hα activity and the measure of its variability are in good agreement with the activity of stellar objects measured with its other parameters, such as X-ray radiation and the mass accretion rate. The EW(Hα) differs not only between objects at different evolutionary stages, but also between variable and non-variable objects. The variables in the CTT and WTT samples are more active than non-variables although they have almost the same evolutionary age. Another distinct difference between these variables and non-variables is their average masses. The variables from both CTT and WTT samples are noticeably more massive than non-variables. Our data confirm the assumption made for other star formation regions that the decay of accretion activity occurs more slowly for more massive CTT objects. Apparently, a similar trend is also present in WTT objects, which are at a later stage of evolution. The variability of the stellar objects, which change their evolutionary classes (CTT ⇆ WTT), at least in a fraction of them, is due to the fact that they are close binaries, which affects and modulates their Hα emission activity.

We use the results of a supernova light-curve population synthesis to predict the range of possible supernova light curves arising from a population of single-star progenitors that lead to type IIP supernovae. We calculate multiple models varying the initial mass, explosion energy, nickel mass and nickel mixing and then compare these to type IIP supernovae with detailed light curve data and pre-explosion imaging progenitor constraints. Where a good fit is obtained to observations, we are able to achieve initial progenitor and nickel mass estimates from the supernova lightcurve that are comparable in precision to those obtained from progenitor imaging. For 2 of the 11 IIP supernovae considered our fits are poor, indicating that more progenitor models should be included in our synthesis or that our assumptions, regarding factors such as stellar mass loss rates or the rapid final stages of stellar evolution, may need to be revisited in certain cases. Using the results of our analysis we are able to show that most of the type IIP supernovae have an explosion energy of the order of log(Eexp/ergs) = 50.52 ± 0.10 and that both the amount of nickel in the supernovae and the amount of mixing may have a dependence on initial progenitor mass.