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Spider pulsars are neutron stars that have a companion star in a close orbit. The companion star sheds material to the neutron star, spinning it up to millisecond rotation periods, while the orbit shortens to hours. The companion is eventually ablated and destroyed by the pulsar wind and radiation 1,2 . Spider pulsars are key for studying the evolutionary link between accreting X-ray pulsars and isolated millisecond pulsars, pulsar irradiation effects and the birth of massive neutron stars 3-6 . Black widow pulsars in extremely compact orbits (as short as 62 minutes 7 ) have companions with masses much smaller than 0.1 M ⊙ . They may have evolved from redback pulsars with companion masses of about 0.1-0.4 M ⊙ and orbital periods of less than 1 day 8 . If this is true, then there should be a population of millisecond pulsars with moderate-mass companions and very short orbital periods 9 , but, hitherto, no such system was known. Here we report radio observations of the binary millisecond pulsar PSR J1953+1844 (M71E) that show it to have an orbital period of 53.3 minutes and a companion with a mass of around 0.07 M ⊙ . It is a faint X-ray source and located 2.5 arcminutes from the centre of the globular cluster M71., (© 2023. The Author(s).)

Fast radio bursts (FRBs) are highly dispersed, millisecond-duration radio bursts 1-3 . Recent observations of a Galactic FRB 4-8 suggest that at least some FRBs originate from magnetars, but the origin of cosmological FRBs is still not settled. Here we report the detection of 1,863 bursts in 82 h over 54 days from the repeating source FRB 20201124A (ref.  9 ). These observations show irregular short-time variation of the Faraday rotation measure (RM), which scrutinizes the density-weighted line-of-sight magnetic field strength, of individual bursts during the first 36 days, followed by a constant RM. We detected circular polarization in more than half of the burst sample, including one burst reaching a high fractional circular polarization of 75%. Oscillations in fractional linear and circular polarizations, as well as polarization angle as a function of wavelength, were detected. All of these features provide evidence for a complicated, dynamically evolving, magnetized immediate environment within about an astronomical unit (AU; Earth-Sun distance) of the source. Our optical observations of its Milky-Way-sized, metal-rich host galaxy 10-12 show a barred spiral, with the FRB source residing in a low-stellar-density interarm region at an intermediate galactocentric distance. This environment is inconsistent with a young magnetar engine formed during an extreme explosion of a massive star that resulted in a long gamma-ray burst or superluminous supernova., (© 2022. The Author(s), under exclusive licence to Springer Nature Limited.)

The dispersive sweep of fast radio bursts (FRBs) has been used to probe the ionized baryon content of the intergalactic medium 1 , which is assumed to dominate the total extragalactic dispersion. Although the host-galaxy contributions to the dispersion measure appear to be small for most FRBs 2 , in at least one case there is evidence for an extreme magneto-ionic local environment 3,4 and a compact persistent radio source 5 . Here we report the detection and localization of the repeating FRB 20190520B, which is co-located with a compact, persistent radio source and associated with a dwarf host galaxy of high specific-star-formation rate at a redshift of 0.241 ± 0.001. The estimated host-galaxy dispersion measure of approximately [Formula: see text] parsecs per cubic centimetre, which is nearly an order of magnitude higher than the average of FRB host galaxies 2,6 , far exceeds the dispersion-measure contribution of the intergalactic medium. Caution is thus warranted in inferring redshifts for FRBs without accurate host-galaxy identifications., (© 2022. The Author(s).)

Fast radio bursts (FRBs) are millisecond-duration radio transients of unknown physical origin observed at extragalactic distances 1-3 . It has long been speculated that magnetars are the engine powering repeating bursts from FRB sources 4-13 , but no convincing evidence has been collected so far 14 . Recently, the Galactic magnetar SRG 1935+2154 entered an active phase by emitting intense soft γ-ray bursts 15 . One FRB-like event with two peaks (FRB 200428) and a luminosity slightly lower than the faintest extragalactic FRBs was detected from the source, in association with a soft γ-ray/hard-X-ray flare 18-21 . Here we report an eight-hour targeted radio observational campaign comprising four sessions and assisted by multi-wavelength (optical and hard-X-ray) data. During the third session, 29 soft-γ-ray repeater (SGR) bursts were detected in γ-ray energies. Throughout the observing period, we detected no single dispersed pulsed emission coincident with the arrivals of SGR bursts, but unfortunately we were not observing when the FRB was detected. The non-detection places a fluence upper limit that is eight orders of magnitude lower than the fluence of FRB 200428. Our results suggest that FRB-SGR burst associations are rare. FRBs may be highly relativistic and geometrically beamed, or FRB-like events associated with SGR bursts may have narrow spectra and characteristic frequencies outside the observed band. It is also possible that the physical conditions required to achieve coherent radiation in SGR bursts are difficult to satisfy, and that only under extreme conditions could an FRB be associated with an SGR burst.

Murine int-2 is one of the genetic loci implicated in the induction of mouse breast cancers by murine mammary tumor virus. An homologous gene has recently been identified in the human genome (Casey et al., 1986). The human int-2 locus was found to be amplified 7- to 25-fold in 4 of 46 infiltrating ductal breast cancers and 30- to 60-fold in 2 of 8 squamous carcinomas of the head and neck region, but not in other cancers. All of the involved tumors had metastasized to regional lymphatics at the time of analysis and five exhibited clinically aggressive behavior.

The incidence of c-ERBB-2 amplification in breast cancers and its usefulness as a predictor of tumor recurrence after treatment have been subjects of controversy (Ali et al., 1988, Slamon et al., 1987). We re-examined this subject by analysing 157 primary and 14 metastatic breast cancers with c-ERBB-2 and 18 other molecular probes as controls. Five proto-oncogenes were found to be occasionally amplified in primary breast cancers: c-ERBB-2 (11%), c-MYB (3%), c-RAS-Ki (3%), INT-2 (4%) and c-MYC (6%). No statistically significant correlation between amplification of c-ERBB-2 and recurrence of tumors was observed. The only significant correlation observed was between early recurrence of advanced (stage III) tumors and amplification of one or another of the above five proto-oncogenes. We conclude that breast cancer utilize multiple genetic mechanisms in their progression and metastasis, and that analysis of c-ERBB-2 alone is not a useful guide.