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ALMA observations of line emission from planet forming discs have demonstrated to be an excellent tool to probe the internal disc kinematics, often revealing subtle effects related to important dynamical processes occurring in them, such as turbulence, or the presence of planets, that can be inferred from pressure bumps perturbing the gas motion, or from the detection of the planetary wake. In particular, we have recently shown for the case of the massive disc in Elias 2-27 as how one can use such kind of observations to measure deviations from Keplerianity induced by the disc self-gravity, thus constraining the total disc mass with good accuracy and independently on mass conversion factors between the tracer used and the total mass. Here, we refine our methodology and extend it to two additional sources, GM Aur and IM Lup, for which archival line observations are available for both the 12CO and the 13CO line. For IM Lup, we are able to obtain a consistent disc mass of |$M_{\rm disc}=0.1 \, \mathrm{M}_{\odot }$|⁠ , implying a disc-star mass ratio of 0.1 (consistent with the observed spiral structure in the continuum emission) and a gas/dust ratio of ∼65 (consistent with standard assumptions), with a systematic uncertainty by a factor of ≃ 2 due to the different methods to extract the rotation curve. For GM Aur, the two lines we use provide slightly inconsistent rotation curves that cannot be attributed only to a difference in the height of the emitting layer, nor to a vertical temperature stratification. Our best-fitting disc mass measurement is |$M_{\rm disc}=0.26 \, \mathrm{M}_{\odot }$|⁠ , implying a disc-star mass ratio of ∼0.35 and a gas/dust ratio of ∼130. Given the complex kinematics in the outer disc of GM Aur and its interaction with the infalling cloud, the CO lines might not well trace the rotation curve and our results for this source should then be considered with some caution. [ABSTRACT FROM AUTHOR]

A growing body of evidence indicates that the star formation rate per unit stellar mass (sSFR) decreases with increasing mass in normal main-sequence star-forming galaxies. Many processes have been advocated as being responsible for this trend (also known as mass quenching), e.g., feedback from active galactic nuclei (AGNs), and the formation of classical bulges. In order to improve our insight into the mechanisms regulating the star formation in normal star-forming galaxies across cosmic epochs, we determine a refined star formation versus stellar mass relation in the local Universe. To this end we use the Hα narrow-band imaging followup survey (Hα3) of field galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Coma and Local superclusters. By complementing this local determination with high-redshift measurements from the literature, we reconstruct the star formation history of main-sequence galaxies as a function of stellar mass from the present epoch up to z = 3. In agreement with previous studies, our analysis shows that quenching mechanisms occur above a threshold stellar mass Mknee that evolves with redshift as ∞(1 + z)2. Moreover, visual morphological classification of individual objects in our local sample reveals a sharp increase in the fraction of visually classified strong bars with mass, hinting that strong bars may contribute to the observed downturn in the sSFR above Mknee. We test this hypothesis using a simple but physically motivated numerical model for bar formation, finding that strong bars can rapidly quench star formation in the central few kpc of field galaxies. We conclude that strong bars contribute significantly to the red colors observed in the inner parts of massive galaxies, although additional mechanisms are likely required to quench the star formation in the outer regions of massive spiral galaxies. Intriguingly, when we extrapolate our model to higher redshifts, we successfully recover the observed redshift evolution for Mknee. Our study highlights how the formation of strong bars in massive galaxies is an important mechanism in regulating the redshift evolution of the sSFR for field main-sequence galaxies. [ABSTRACT FROM AUTHOR]

d-Amphetamine (d-AMP) is a potent releaser of dopamine (DA), and its central nervous system stimulant action is mediated primarily through its effect on the substantia nigra and ventral tegmental area dopaminergic neurons (nuclei A9 and A10, respectively). The purpose of the present experiment was to use electrophysiological techniques to examine dendritic release of DA in the in vitro slice preparation, and determine whether: (1) d-AMP inhibits the firing rates of both A9 and A10 cells; (2) the d-AMP-induced inhibition is mediated via the dendritic release of DA; and (3) there is spontaneous dendritic release of DA. Superfusion with d-AMP (2-100 μM) produced identical inhibitory dose-response curves for A9 and A10 cells, and a dose of 6.25 μM caused more than 50% inhibition in the cell firing rates. The d-AMP-induced inhibition was attenuated by blocking DA synthesis. Either D2 receptor blockade (sulpiride, 1 μM), or DA synthesis inhibition (α-methylparatyrosine, 50 μM) resulted in a marked increase in the firing rates of dopaminergic cells. These data suggest that d-AMP comparably releases DA from both A9 and A10 cell dendrites, that it releases newly-synthesized DA to inhibit cell firing, and that DA is tonically released to regulate cell firing rates via interactions with inhibitory D2 autoreceptors. [ABSTRACT FROM AUTHOR]