Narrow-line Seyfert 1 (NLS1) galaxies are a peculiar subclass of activegalactic nuclei (AGN). They have demonstrated that the presence of relativisticjets in an AGN is not strictly related to its radio-loudness, the black holemass, or the host galaxy type. Here we present a remarkable example of aradio-quiet NLS1, 6dFGS gJ035432.8-134008 (J0354-1340). In our Karl G. JanskyVery Large Array observations at 5.5 GHz the source shows a bright core with aflat spectral index, and extended emission corresponding to very elongatedjets. These are the largest double-sided radio jets found to date in an NLS1,with a deprojected linear size of almost 250 kpc. We also analysednear-infrared and optical images obtained by the Magellan Baade and theEuropean Southern Observatory New Technology Telescope. By means of photometricdecomposition and colour maps, we determined that J0354-1340 is hosted by aspiral/disk galaxy. Fully evolved relativistic jets have traditionally beenassociated with high-mass elliptical galaxies hosting the most massive blackholes, but our results confirm that also less massive black holes in spiralgalaxies can launch and sustain powerful jets, implying that the launching ofthe jets is governed by factors other than previously believed.

We present ALMA observations at a spatial resolution of 0.2 arcsec (60 pc) ofCO emission from the Taffy galaxies (UGC 12914/5). The observations arecompared with narrow-band Pa$\alpha$, mid-IR, radio continuum and X-rayimaging, plus optical spectroscopy. The galaxies have undergone a recenthead-on collision, creating a massive gaseous bridge which is known to behighly turbulent. The bridge contains a complex web of narrow molecularfilaments and clumps. The majority of the filaments are devoid of starformation, and fall significantly below the Kennicutt-Schmidt relationship fornormal galaxies, especially for the numerous regions undetected in Pa$\alpha$emission. Within the loosely connected filaments and clumps of gas we findregions of high velocity dispersion which appear gravitationally unbound for awide range of likely values of $X_{\rm CO}$. Like the "Firecracker" region inthe Antennae system, they would require extremely high external dynamical orthermal pressure to stop them dissipating rapidly on short crossing timescalesof 2-5~Myrs. We suggest that the clouds may be transient structures within ahighly turbulent multi-phase medium which is strongly suppressing starformation. Despite the overall turbulence in the system, stars seem to haveformed in compact hotspots within a kpc-sized extragalactic HII region, wherethe molecular gas has a lower velocity dispersion than elsewhere, and showsevidence for a collision with an ionized gas cloud. Like the shocked gas in theStephan's Quintet group, the conditions in the Taffy bridge shows how difficultit is to form stars within a turbulent, multi-phase, gas.

Current 3D object detectors for autonomous driving are almost entirelytrained on human-annotated data. Although of high quality, the generation ofsuch data is laborious and costly, restricting them to a few specific locationsand object types. This paper proposes an alternative approach entirely based onunlabeled data, which can be collected cheaply and in abundance almosteverywhere on earth. Our approach leverages several simple common senseheuristics to create an initial set of approximate seed labels. For example,relevant traffic participants are generally not persistent across multipletraversals of the same route, do not fly, and are never under ground. Wedemonstrate that these seed labels are highly effective to bootstrap asurprisingly accurate detector through repeated self-training without a singlehuman annotated label.

Using sedimentary and eclipse-based measurements of the lunar recessionvelocity, we derive a new local-Universe measurement of the Hubble constant($H_0$) from the recession rate of Earth's Moon. Taking into account theeffects of tides, we find a value of $H_{0}$ = 63.01 $\pm$ 1.79 km s$^{-1}$Mpc$^{-1}$, which is in approximate agreement with the Planck space mission'smeasurement using the cosmic microwave background (CMB) and base $\Lambda$CDM.Our new measurement represents the first ever model-independent, single-stepmeasurement of the Universe's current expansion rate. This is also the firstmajor local Universe measurement of $H_0$ which is below the measurement fromPlanck. Importantly, it is robust to the systematic errors that may be presentin other $H_0$ measurements using other cosmological probes such as type Iasupernovae, baryon acoustic oscillations, or lensed quasars. Our work provideskey evidence towards the notion that the existing Hubble tension may indeed bea result of systematic uncertainties in the local distance ladder.

The Javalambre-Physics of the Accelerating Universe Astrophysical Survey(J-PAS) is expected to map thousands of square degrees of the northern sky with56 narrowband filters in the upcoming years. This will make J-PAS a verycompetitive and unbiased emission line survey compared to spectroscopic ornarrowband surveys with fewer filters. The miniJPAS survey covered 1 deg$^2$,and it used the same photometric system as J-PAS, but the observations werecarried out with the pathfinder J-PAS camera. In this work, we identify andcharacterize the sample of emission line galaxies (ELGs) from miniJPAS with aredshift lower than $0.35$. Using a method based on artificial neural networks,we detect the ELG population and measure the equivalent width and flux of the$H\alpha$, $H\beta$, [OIII], and [NII] emission lines. We explore theionization mechanism using the diagrams [OIII]/H$\beta$ versus [NII]/H$\alpha$(BPT) and EW(H$\alpha$) versus [NII]/H$\alpha$ (WHAN). We identify 1787 ELGs($83$%) from the parent sample (2154 galaxies) in the AEGIS field. For thegalaxies with reliable EW values that can be placed in the WHAN diagram (2000galaxies in total), we obtained that $72.8 \pm 0.4$%, $17.7 \pm 0.4$% , and$9.4 \pm 0.2$% are star-forming (SF), active galactic nucleus (Seyfert), andquiescent galaxies, respectively. Based on the flux of $H\alpha$ we find thatthe star formation main sequence is described as $\log$ SFR $[M_\mathrm{\odot}\mathrm{yr}^{-1}] = 0.90^{+ 0.02}_{-0.02} \log M_{\star} [M_\mathrm{\odot}]-8.85^{+ 0.19}_{-0.20}$ and has an intrinsic scatter of $0.20^{+0.01}_{-0.01}$. The cosmic evolution of the SFR density ($\rho_{\text{SFR}}$)is derived at three redshift bins: $0 < z \leq 0.15$, $0.15 < z \leq 0.25$, and$0.25 < z \leq 0.35$, which agrees with previous results that were based onmeasurements of the $H\alpha$ emission line.