Context. Complex organic species are known to be abundant toward low-and high-mass protostars. No statistical study of these species toward a large sample of high-mass protostars with the Atacama Large Millimeter/submillimeter Array (ALMA) has been carried out so far. Aims. We aim to study six N-bearing species: methyl cyanide (CH 3 CN), isocyanic acid (HNCO), formamide (NH 2 CHO), ethyl cyanide (C 2 H 5 CN), vinyl cyanide (C 2 H 3 CN) and methylamine (CH 3 NH 2 ) in a large sample of line-rich high-mass protostars. Methods. From the ALMA Evolutionary study of High Mass Protocluster Formation in the Galaxy survey, 37 of the most line-rich hot molecular cores with ∼1 angular resolution are selected. Next, we fit their spectra and find column densities and excitation temperatures of the N-bearing species mentioned above, in addition to methanol (CH 3 OH) to be used as a reference species. Finally, we compare our column densities with those in other low-and high-mass protostars. Results. CH 3 OH, CH 3 CN and HNCO are detected in all sources in our sample, whereas C 2 H 3 CN and CH 3 NH 2 are (tentatively) detected in ∼78% and ∼32% of the sources. We find three groups of species when comparing their excitation temperatures: hot (NH 2 CHO; T ex 250 K), warm (C 2 H 3 CN, HN 13 CO and CH 13 3 CN; 100 K T ex 250 K) and cold species (CH 3 OH and CH 3 NH 2 ; T ex 100 K). This temperature segregation reflects the trend seen in the sublimation temperature of these molecules and validates the idea that complex organic emission shows an onion-like structure around protostars. Moreover, the molecules studied here show constant column density ratios across low-and high-mass protostars with scatter less than a factor ∼3 around the mean. Conclusions. The constant column density ratios point to a common formation environment of complex organics or their precursors, most likely in the pre-stellar ices. The scatter around the mean of the ratios, although small, varies depending on the species considered. This spread can either have a physical origin (source structure, line or dust optical depth) or a chemical one. Formamide is most prone to the physical effects as it is tracing the closest regions to the protostars, whereas such effects are small for other species. Assuming that all molecules form in the pre-stellar ices, the scatter variations could be explained by differences in lifetimes or physical conditions of the pre-stellar clouds. If the pre-stellar lifetimes are the main factor, they should be similar for low-and high-mass protostars (within factors ∼2 − 3).

We investigated the relationship between F-actin damage and cell detachment using nephrotoxic L-cysteine S-conjugates. In vivo S-(1,2-dichlorovinyl)-L-cysteine (DCVC) induced loss of F-actin in the S3 segment of the proximal tubule in the outer stripe of the outer medulla, which was associated with loss of the brush border and loss of cells from the basement membrane. In vitro DCVC caused the detachment of primary cultured rat renal proximal tubular cells (PTC), which was clearly associated with F-actin damage. Disorganization of F-actin correlated with an increase in cellular levels of G-actin, indicating depolymerization of F-actin. Cell detachment was preceded by a complete loss of the alpha-actinin binding protein talin from the focal adhesions, which was directly associated with F-actin disorganization. Inhibition of formation of highly reactive metabolites from L-cysteine S-conjugates by L-cysteine-S-conjugate beta-lyase completely prevented both F-actin damage and cell detachment by DCVC. Although inhibition of DCVC-induced lipid peroxidation and reduction of intracellular free calcium by N,N'-diphenyl-p-phenylenediamine and the acetoxymethyl ester of ethylene glycol-bis(beta-aminoethyl ether)-N,N,N',N'-tetraacetic acid, respectively, clearly prevented cell death, no protection was observed against the DCVC-induced F-actin disorganization, talin redistribution, and cell detachment. Also, F-actin damage was unrelated to changes in the energy status of the PTC, since cellular ATP content was unaffected. The data clearly demonstrate a close relationship between F-actin damage, disturbances of focal adhesions, and cell detachment. In addition, different molecular pathways are involved in the cell detachment caused by F-actin disorganization and initiation of cell death.

Context. The deuteration of molecules forming in the ices such as methanol (CH 3 OH) is sensitive to the physical conditions during their formation in dense cold clouds and can be probed through observations of deuterated methanol in hot cores. Aims. The aim is to determine the D/H ratio of methanol for a large sample of 99 high-mass protostars and to link this to the physical conditions during the formation of methanol in the prestellar phases. Methods. Observations with the Atacama Large Millimeter/submillimeter Array (ALMA) containing transitions of CH 3 OH, CH 2 DOH, CHD 2 OH, 13 CH 3 OH, and CH 18 3 OH are investigated. The column densities of CH 2 DOH, CHD 2 OH, and CH 3 OH are determined for all sources, where the column density of CH 3 OH is derived from optically thin 13 C and 18 O isotopologues. Consequently, the D/H ratio of methanol is derived taking statistical effects into account. Results. Singly deuterated methanol (CH 2 DOH) is detected at the 3σ level toward 25 of the 99 sources in our sample of the highmass protostars. Including upper limits, the (D/H) CH 3 OH ratio inferred from N CH 2 DOH /N CH 3 OH was derived for 38 of the 99 sources and varies between ∼ 10 −3 − 10 −2 . Including other high-mass hot cores from the literature, the mean methanol D/H ratio is 1.1 ± 0.7 × 10 −3 . This is more than one order of magnitude lower than what is seen for low-mass protostellar systems (2.2 ± 1.2 × 10 −2 ). Doubly deuterated methanol (CHD 2 OH) is detected at the 3σ level toward 11 of the 99 sources. Including upper limits for 15 sources, the (D/H) CH 2 DOH ratios derived from N CHD 2 OH /N CH 2 DOH are more than two orders of magnitude higher than (D/H) CH 3 OH with an average of 2.0 ± 0.8 × 10 −1 which is similar to what is found for low-mass sources. Comparison with literature GRAINOBLE models suggests that the high-mass prestellar phases are either warm (> 20 K) or live shorter than the free-fall timescale. In contrast, for low-mass protostars, both a low temperature of < 15 K and a prestellar phase timescale longer than the free-fall timescale are necessary. Conclusions. The (D/H) CH 3 OH ratio drops by more than an order of magnitude between low-mass and high-mass protostars due to either a higher temperature during the prestellar phases or shorter prestellar phases. However, successive deuteration toward CHD 2 OH seems equally effective between low-mass and high-mass systems.