As we collectively welcome the new year, we retrace the 2020 milestones in sample return and look at a few of the major upcoming events in 2021. There are many reasons for astronomers to be optimistic.

HORuS, a new high-resolution spectrograph for the Gran Telescopio Canarias, will facilitate an expanded range of optical and near-infrared studies, explains Instrument Scientist Carlos Allende Prieto.

Magnetars are the most highly magnetized neutron stars in the cosmos (with magnetic field 1013–1015 G). Giant flares from magnetars are rare, short-duration (about 0.1 s) bursts of hard X-rays and soft γ rays1,2. Owing to the limited sensitivity and energy coverage of previous telescopes, no magnetar giant flare has been detected at gigaelectronvolt (GeV) energies. Here, we report the discovery of

The largest ever simulation of astrophysical turbulence substantially improves our understanding of how energy injection on large interstellar scales governs how stars form on small scales.

Benzonitrile (c-C6H5CN, where ‘c’ indicates a cyclic structure), a polar proxy for benzene (c-C6H6), has the potential to serve as a highly convenient radio probe for aromatic chemistry, provided that this ring can be found in other astronomical sources beyond the molecule-rich prestellar cloud TMC-1. Here we present radio astronomical evidence of benzonitrile in four other prestellar, and possibly

Feedback-driven winds from star formation or active galactic nuclei might be a relevant channel for the abrupt quenching of star formation in massive galaxies. However, both observations and simulations support the idea that these processes are non-conflictingly co-evolving and self-regulating. Furthermore, evidence of disruptive events that are capable of fast quenching is rare, and constraints on

Understanding the physics of turbulence is crucial for many applications, including weather, industry and astrophysics. In the interstellar medium1,2, supersonic turbulence plays a crucial role in controlling the gas density and velocity structure, and ultimately the birth of stars3,4,5,6,7,8. Here we present a simulation of interstellar turbulence with a grid resolution of 10,0483 cells that allows

As the inventory of interstellar molecules continues to grow, the gulf between small species, whose individual rotational lines can be observed with radio telescopes, and large ones, such as polycyclic aromatic hydrocarbons best studied in bulk via infrared and optical observations, is slowly being bridged. Understanding the connection between these two molecular reservoirs is critical to understanding

Analyses of meteorites and theoretical models indicate that some carbonaceous near-Earth asteroids may have been thermally altered due to radiative heating during close approaches to the Sun1,2,3. However, the lack of direct measurements on the subsurface doesn’t allow us to distinguish thermal alteration due to radiative heating from parent-body processes. In April 2019, the Hayabusa2 mission successfully

A Correction to this paper has been published: https://doi.org/10.1038/s41550-020-01293-w

Carbonaceous chondrite meteorites record the earliest stages of Solar System geological activities and provide insight into their parent bodies’ histories. Some carbonaceous chondrites are volumetrically dominated by hydrated minerals, providing evidence for low-temperature, low-pressure aqueous alteration1. Others are dominated by anhydrous minerals and textures that indicate high-temperature metamorphism

Pluto, Titan and Triton all have low-temperature environments with an N2, CH4 and CO atmospheric composition in which solar radiation drives an intense organic photochemistry. Titan is rich in atmospheric hazes, and Cassini–Huygens observations showed that their formation is initiated with the production of large molecules through ion-neutral reactions. New Horizons revealed that optical hazes are

Low-mass stars show evidence of vigorous magnetic activity in the form of large flares and coronal mass ejections. Such space weather events may have important ramifications for the habitability and observational fingerprints of exoplanetary atmospheres. Here, using a suite of three-dimensional coupled chemistry–climate model simulations, we explore effects of time-dependent stellar activity on rocky

The formation and evolutionary processes of galaxy bulges are still unclear, and the presence of young stars in the bulge of the Milky Way is largely debated. We recently demonstrated that Terzan 5, in the Galactic bulge, is a complex stellar system hosting stars with very different ages and a striking chemical similarity to the field population. This indicates that its progenitor was probably one

GN-z11 was photometrically selected as a luminous star-forming galaxy candidate at redshift z > 10 on the basis of Hubble Space Telescope imaging data1. Follow-up Hubble Space Telescope near-infrared grism observations detected a continuum break that was explained as the Lyα break corresponding to \(z = 11.09_{ - 0.12}^{ + 0.08}\) (ref. 2). However, its accurate redshift remained unclear. Here we report

In the optical sky, minutes-duration transients from cosmological distances are rare. Known objects that give rise to such transients include gamma-ray bursts (GRBs), the most luminous explosions in the Universe1 that have been detected at redshifts as high as z ≈ 9.4 (refs. 2,3,4). These high-redshift GRBs and their associated emission can be used to probe the star formation and reionization history

The discovery of giant X-ray bubbles above and below the centre of the Milky Way confirms that the central supermassive black hole was once more than 100 million times brighter than its current state.

The BICEP Array will bring a new level of sensitivity to observations of cosmic microwave background polarization patterns on large angular scales, says Clem Pryke on behalf of the BICEP/Keck Collaboration.

The ‘new normal’ way of life for coping with the COVID-19 outbreak is a work in progress. When we move on, we should keep some of our adaptations rather than return to the old ways, for a more open and equitable way of working.

The ultraviolet emission from the solar transition region is dominated by dynamic, low-lying magnetic loops. The enhanced spatial and temporal resolution of the solar observation satellite Interface Region Imaging Spectrograph (IRIS) has made it possible to study these structures in fine detail. IRIS has observed ‘transient brightenings’ in these loops, associated with strong excess line broadenings1

The directions of the galaxy angular momenta can be predicted from the initial conditions of the early Universe through the tidal torque. In simulations, these directions are well preserved through cosmic time, consistent with expectations of angular momentum conservation. We find evidence, statistically significant at ~3σ, of correlation between observed oriented directions of galaxy angular momentum

Outflows from active galactic nuclei (AGNs) are one of the fundamental mechanisms by which the central supermassive black hole interacts with its host galaxy. Detected in ≥50% of nearby AGNs, these outflows have been found to carry kinetic energy that is a large fraction of the AGN power, and thereby give ‘negative’ feedback to their host galaxies. To understand the physical processes that regulate

One of the giants of planetary science, H. J. Melosh, died unexpectedly on 11 September 2020 at age 73. Through his students, postdocs and collaborators, he brought a high level of physical rigour to the growing field of planetary geology.

The Large Magellanic Cloud is the most massive satellite galaxy of the Milky Way, with an estimated mass exceeding a tenth of the mass of the Milky Way1,2,3,4,5. Just past its closest approach of about 50 kpc, and flying past the Milky Way at an astonishing speed of 327 km s−1 (ref. 6), the Large Magellanic Cloud can affect our Galaxy in a number of ways, including dislodging the Milky Way disk from

Fast radio bursts are millisecond-duration, bright radio signals (fluence 0.1–100 Jy ms) emitted from extragalactic sources of unknown physical origin. The recent CHIME/FRB and STARE2 detection of an extremely bright (fluence ~MJy ms) radio burst from the Galactic magnetar SGR 1935+2154 supports the hypothesis that (at least some) fast radio bursts are emitted by magnetars at cosmological distances

The detection of the amino acid glycine and its amine precursor methylamine on the comet 67P/Churyumov-Gerasimenko by the Rosetta mission provides strong evidence for a cosmic origin of amino acids on Earth. How and when such molecules form along the process of star formation remains debated. Here we report the laboratory detection of glycine formed in the solid phase through atom and radical–radical

Govind Swarup was a pioneer in the field of radio astronomy and the driving force behind two innovative Indian radio telescopes. He contributed significantly to building up research institutions and promoting science education and training programs in the country.

The bombardment of impactors (leftover planetesimals, asteroids and comets) created numerous impact craters on the Moon. The giant planets in the outer Solar System are believed to have experienced a dynamical instability, in which the migration of giant planets delivers impactors to the inner Solar System bodies1,2. The difference between the population of large (diameter more than ~5 km) impact craters

Europa’s surface continuously experiences high fluxes of charged particles due to the presence of Jupiter’s strong magnetic field. These high-energy charged particles, including electrons, interact with the ice- and salt-rich surface, resulting in complex physical and chemical processes. Here, we report that Europa ice analogues emit characteristic spectral signatures in the visible region when exposed

The Colorado Ultraviolet Transit Experiment CubeSat mission aims to observe atmospheric escape from a dozen or more exoplanets by monitoring them in the near-ultraviolet, explains Principal Investigator Kevin France.

High-performance scientific satellites are currently the exclusive domain of government-funded agencies. The team behind the Twinkle Space Mission is developing a new class of small and sustainable science satellites that leverages recent innovations in the commercial space sector.

Small satellites are revolutionizing the way we access space for commerce and science, including astronomy and planetary science. Yet, like many breakthrough technologies, it has a double-edge.

Earth’s exosphere is set to become increasingly crowded, with tens of thousands of commercial telecommunication satellites planned in the next few years. We need to ensure that technological and socio-economic advancements will not imperil scientific progress and humanity’s access to dark skies.

The development of small satellites for telecommunication constellations in low-Earth orbit provides a unique opportunity to the astronomical community. Mass-produced, commercial satellite platforms can host dedicated scientific payloads and expand access to space-based astronomy. Technologies critical to the development of small orbital instruments have been demonstrated by exploratory missions. By

At the dawn of the space age, nanosatellites, weighing between 1 and 10 kg, were used because of launcher limitations. In the past twenty years, a renaissance has occurred as a consequence of the success of microsatellites in accessing auxiliary and piggyback launch opportunities driving affordability. In addition, the capabilities and flight demonstrations of microelectronics components in orbit and

Near-Earth space is becoming increasingly privatized, with the number of satellites in low-Earth orbits predicted to grow dramatically from about 2,000 at present to over 100,000 in the next decade due to the launch of planned satellite constellations. In addition to their direct impact on astronomy, the manner and pace of ‘occupying’ near-Earth space raises the risk of repeating the mistakes of colonization

The number of small satellites has grown hugely in the past decade, from tens of satellites per year in the mid-2010s to a projection of tens of thousands in orbit by the mid-2020s. This presents both problems and opportunities for observational astronomy. Small satellites offer complementary cost-effective capabilities to both ground-based astronomy and larger space missions. Compared with ground-based

Radio observations from the Low Frequency Radio Array suggest that magnetic fields in high-redshift clusters are of similar strength as their local counterparts. This finding implies that magnetic fields evolve differently than predicted by cosmological simulations.

In the present-day Universe, magnetic fields pervade galaxy clusters1 and have strengths of a few microgauss, as measured from Faraday rotation2. Evidence for cluster magnetic fields is also provided by the observation of megaparsec-scale radio emission, namely radio halos and relics3. These are commonly found in merging systems4 and are characterized by a steep radio spectrum Sν (α < −1, where Sν

Multi-messenger astronomy, the coordinated observation of different classes of signals that originate from the same astrophysical event, provides a wealth of information about astrophysical processes1. So far, multi-messenger astronomy has correlated signals from known fundamental forces and standard model particles like electromagnetic radiation, neutrinos and gravitational waves. Many of the open

Widespread hydration was detected on the lunar surface through observations of a characteristic absorption feature at 3 µm by three independent spacecraft1,2,3. Whether the hydration is molecular water (H2O) or other hydroxyl (OH) compounds is unknown and there are no established methods to distinguish the two using the 3 µm band4. However, a fundamental vibration of molecular water produces a spectral

Jellyfish galaxies have long tails of gas that is stripped from the disk by ram pressure due to the motion of galaxies in the intracluster medium in galaxy clusters. Here, we present the magnetic field strength and orientation within the disk and the (90-kpc-long) Hα-emitting tail of the jellyfish galaxy JO206. The tail has a large-scale magnetic field (>4.1 μG), a steep radio spectral index (α ≈ −2

Water ice is thought to be trapped in large permanently shadowed regions in the Moon’s polar regions, due to their extremely low temperatures. Here, we show that many unmapped cold traps exist on small spatial scales, substantially augmenting the areas where ice may accumulate. Using theoretical models and data from the Lunar Reconnaissance Orbiter, we estimate the contribution of shadows on scales

An amendment to this paper has been published and can be accessed via a link at the top of the paper.

Finding the basic mechanism governing the surface history of asteroids of various shapes is essential for understanding their origin and evolution. In particular, the asteroids (162173) Ryugu1 and (101955) Bennu2 currently being visited by Hayabusa2 and OSIRIS-REx appear to be top shaped. This distinctive shape, characterized by a raised equatorial bulge, is shared by other similarly sized asteroids

The Milky Way galaxy is surrounded by a circumgalactic medium1 that may play a key role in galaxy evolution as the source of gas for star formation and a repository of metals and energy produced by star formation and nuclear activity2. The circumgalactic medium may also be a repository for baryons seen in the early universe, but undetected locally3. The circumgalactic medium has an ionized component

Astronomy research in Malaysia has progressed rapidly in the last few decades, with an increasing number of enthusiastic Malaysian astronomers working together to build new research groups and observing facilities, while establishing research networks both locally and globally.

An amendment to this paper has been published and can be accessed via a link at the top of the paper.

An amendment to this paper has been published and can be accessed via a link at the top of the paper.

On a magnetar’s surface, magnetic fields can create permanent sunspot-like structures. Accounting for heat diffusion and magnetic evolution in a magnetar’s crust in the latest simulations improves agreement with observations.

Magnetars are neutron stars (NSs) with extreme magnetic fields1 of strength 5 × 1013−1015 G. These fields are generated by dynamo action during the proto-NS phase, and are expected to have both poloidal and toroidal components2,3,4,5,6, although the energy of the toroidal component could be ten times larger7. Only the poloidal dipolar field can be measured directly, via NS spin-down8. The magnetic

Comparing microphysical models of aerosol production to Hubble Space Telescope transit spectra reveals a surprisingly simple transition between atmospheres with hydrocarbon hazes, silicate clouds and clear skies.

Philanthropic donations are a significant contribution to the betterment of humankind, with a large percentage dedicated to science and education. Affordable small satellites may offer philanthropists the opportunity to give students and underprivileged communities access to small space telescopes.

The Space Academic Network made a case for a small-satellite programme for the United Kingdom to provide access to space, and a route for advancing science and technology; however, funding has not been forthcoming. The search for a killer argument for this widely supported programme continues.

The detection of phosphine in the cloud decks of Venus generated 4,700 news stories around the world. This kind of coordination was only possible because of our embargo policy.

In its 16 years of scientific measurements, the Spitzer Space Telescope performed ground-breaking and key infrared measurements of Solar System objects near and far. Targets ranged from the smallest planetesimals to the giant planets; Spitzer helped us to reshape our understanding of these objects while also laying the groundwork for future infrared space-based observations like those to be undertaken

In its 16 years of scientific measurements, the Spitzer Space Telescope performed a number of groundbreaking and key infrared measurements of Solar System objects near and far. In this second of two Review Articles, we describe results from Spitzer observations of asteroids, dust rings and planets that provide new insight into the formation and evolution of our Solar System. The key Spitzer results

An amendment to this paper has been published and can be accessed via a link at the top of the paper.

The New Horizons spacecraft’s flyby of Kuiper belt object (486958) Arrokoth revealed a bilobed shape with highly flattened lobes both aligned to its equatorial plane, and a rotational axis almost aligned to the orbital plane (obliquity ~99°)1,2,3,4. Arrokoth belongs to the cold classical Kuiper belt object population that occupies dynamically undisturbed orbits around the Sun, and as such is a primitive

Lithium has confused scientists for decades at almost every scale of the universe. Lithium-rich giants are peculiar stars with lithium abundances greater than model prediction. A large fraction of lithium-rich low-mass evolved stars are traditionally supposed to be red giant branch (RGB) stars. Recent studies, however, report that red clump (RC) stars are more frequent than RGB stars. Here, we present