Effects of physical and social environment on zebra finches’ foraging intensity

The zebra finch (Taeniopygia guttata) is the most widely used passerine bird in captive research, yet little work has been done in the wild where physical and social conditions are more variable and their behaviour can be investigated in an ecological context. Zebra finches forage on the ground and are vulnerable to predation by a range of terrestrial and aerial predators. In this thesis, I explore how the physical and social environment affects their foraging decisions in captivity and in the wild. The decision to feed in a particular patch is an attempt to optimise the costs and benefits of feeding at that location. I used giving-up densities (GUD) – the density of food remaining in a patch after the forager(s) have exploited it, to measure the perceived risk of zebra finches to a variety of experimental treatments. In captivity, I investigated how zebra finches’ foraging intensity responded to characteristics of the captive environment such as the availability of perches, cover, and ground substrate. In the wild, I examined how their foraging intensity was affected by the distance to natural cover (vegetation) or their visual fields. I also explored effects of the local neighbourhood density of zebra finches in the wild. I further investigated captive zebra finches’ foraging intensity in different sized groups, as a function of the proximity to, and behaviour of neighbouring flocks. I show that zebra finches forage more intensively when they are close to vegetation and perceive cover as protective. I also found that foraging intensity increased non-linearly with group size and mass and sex mitigated how social and physical environments affected foraging intensity. Overall, my finding suggest that while foraging, zebra finches place greater emphasis on their social, compared to physical environments. My thesis highlights the importance of taking into account a wide range of social factors when investigating foraging decisions by animals

Trigonometric Parallaxes of Massive Star Forming Regions: G012.88+0.48 and W33

We report trigonometric parallaxes for water masers in the G012.88+0.48 region and in the massive star forming complex W33 (containing G012.68--0.18, G012.81--0.19, G012.90--0.24, G012.90--0.26), from the Bar and Spiral Structure Legacy (BeSSeL) survey using the Very Long Baseline Array. The parallax distances to all these masers are consistent with $2.40^{+0.17}_{-0.15}$ kpc, which locates the W33 complex and G012.88+0.48 in the Scutum spiral arm. Our results show that W33 is a single star forming complex at about two-thirds the kinematic distance of 3.7 kpc. The luminosity and mass of this region, based on the kinematic distance, have therefore been overestimated by more than a factor of two. The spectral types in the star cluster in W33\,Main have to be changed by 1.5 points to later types.Comment: 9 pages, 11 figures, 2 tables; accepted for publication at A&

The Parallax of W43: a Massive Star Forming Complex near the Galactic Bar

We report trigonometric parallax measurements of masers in the massive star forming complex W43 from VLBA observations as part of the BeSSeL Survey. Based on measurements of three 12 GHz methanol maser sources (G029.86-00.04, G029.95-00.01 and G031.28+00.06) and one 22 GHz water maser source (G031.58+00.07) toward W43, we derived a distance of $5.49^{+0.39}_{-0.34}$ kpc to W43. By associating the masers with CO molecular clouds, and associating the clouds kinematically with CO longitude-velocity spiral features, we assign W43 to the Scutum spiral arm, close to the near end of the Galactic bar. The peculiar motion of W43 is about 20 km/s toward the Galactic Center and is very likely induced by the gravitational attraction of the bar.Comment: 23 pages, 16 figures, accepted for publication in Ap

Learning Layer-wise Equivariances Automatically using Gradients

Convolutions encode equivariance symmetries into neural networks leading to better generalisation performance. However, symmetries provide fixed hard constraints on the functions a network can represent, need to be specified in advance, and can not be adapted. Our goal is to allow flexible symmetry constraints that can automatically be learned from data using gradients. Learning symmetry and associated weight connectivity structures from scratch is difficult for two reasons. First, it requires efficient and flexible parameterisations of layer-wise equivariances. Secondly, symmetries act as constraints and are therefore not encouraged by training losses measuring data fit. To overcome these challenges, we improve parameterisations of soft equivariance and learn the amount of equivariance in layers by optimising the marginal likelihood, estimated using differentiable Laplace approximations. The objective balances data fit and model complexity enabling layer-wise symmetry discovery in deep networks. We demonstrate the ability to automatically learn layer-wise equivariances on image classification tasks, achieving equivalent or improved performance over baselines with hard-coded symmetry

Risk factors for secondary dilatation of the aorta after acute type A aortic dissection

Objectives: Prompt diagnosis of subsequent dilatation of the dissected aorta is crucial to reduce late mortality in these patients. This study focuses on risk factors for dilatation of the aorta after type A aortic dissection (AADA) affecting a normal-sized or slightly dilated aorta. Methods: Overall 531 CT scans were analysed. Patients were included in the study if at least 3 CT scans were available after operative repair. 64 patients (59.8%) out of 107 patients full-field the inclusion criteria. Volumetric analyses of the aorta were performed. Patients were divided in 3 groups: group A included 26 patients (40.6%) without progression of the aortic diameter, group 2, 27 patients (42.2%) with slight progression and group 3, 11 patients (17.2%) with important progression, requiring surgery in 9 patients (81.8%). Risk-factors for progression of the aortic size were analysed and compared between the groups. Results: Patients from group 3 were younger 57.7±13.4 vs. 61.9±11.6 in group 1 (P≪0.05) and were more frequent female (45.4 vs. 23.1%; P≪0.05). Dissection of the supraaortic branches (100 vs. 80.8%; P≪0.05), the presence of preoperative cerebral, visceral or peripheral malperfusion (54.6 vs. 26.9%; P≪0.05) and contrast enhancement in the false lumen during the follow-up (72.7 vs. 57.7%; P=0.07) were additional risk factors for late aortic dilatation in these patients. Conclusions: Acute type A aortic dissection in younger patients, involving the supraaortic branches and/or combined with malperfusion syndrome favour secondary dilatation. A close follow-up is mandatory to prevent acute complications of the diseased downstream aorta following repair of a AAD

Techniques for Accurate Parallax Measurements for 6.7-GHz Methanol Masers

The BeSSeL Survey is mapping the spiral structure of the Milky Way by measuring trigonometric parallaxes of hundreds of maser sources associated with high-mass star formation. While parallax techniques for water masers at high frequency (22 GHz) have been well documented, recent observations of methanol masers at lower frequency (6.7 GHz) have revealed astrometric issues associated with signal propagation through the ionosphere that could significantly limit parallax accuracy. These problems displayed as a "parallax gradient" on the sky when measured against different background quasars. We present an analysis method in which we generate position data relative to an "artificial quasar" at the target maser position at each epoch. Fitting parallax to these data can significantly mitigate the problems and improve parallax accuracy

Risk factors for secondary dilatation of the aorta after acute type A aortic dissection

Objectives: Prompt diagnosis of subsequent dilatation of the dissected aorta is crucial to reduce late mortality in these patients. This study focuses on risk factors for dilatation of the aorta after type A aortic dissection (AADA) affecting a normal-sized or slightly dilated aorta. Methods: Overall 531 CT scans were analysed. Patients were included in the study if at least 3 CT scans were available after operative repair. 64 patients (59.8%) out of 107 patients full-field the inclusion criteria. Volumetric analyses of the aorta were performed. Patients were divided in 3 groups: group A included 26 patients (40.6%) without progression of the aortic diameter, group 2, 27 patients (42.2%) with slight progression and group 3, 11 patients (17.2%) with important progression, requiring surgery in 9 patients (81.8%). Risk-factors for progression of the aortic size were analysed and compared between the groups. Results: Patients from group 3 were younger 57.7±13.4 vs. 61.9±11.6 in group 1 (P≪0.05) and were more frequent female (45.4 vs. 23.1%; P≪0.05). Dissection of the supraaortic branches (100 vs. 80.8%; P≪0.05), the presence of preoperative cerebral, visceral or peripheral malperfusion (54.6 vs. 26.9%; P≪0.05) and contrast enhancement in the false lumen during the follow-up (72.7 vs. 57.7%; P=0.07) were additional risk factors for late aortic dilatation in these patients. Conclusions: Acute type A aortic dissection in younger patients, involving the supraaortic branches and/or combined with malperfusion syndrome favour secondary dilatation. A close follow-up is mandatory to prevent acute complications of the diseased downstream aorta following repair of a AADA

Trigonometric Parallaxes of High Mass Star Forming Regions: the Structure and Kinematics of the Milky Way

Over 100 trigonometric parallaxes and proper motions for masers associated with young, high-mass stars have been measured with the BeSSeL Survey, a VLBA key science project, the EVN, and the Japanese VERA project. These measurements provide strong evidence for the existence of spiral arms in the Milky Way, accurately locating many arm segments and yielding spiral pitch angles ranging from 7 to 20 degrees. The widths of spiral arms increase with distance from the Galactic center. Fitting axially symmetric models of the Milky Way with the 3-D position and velocity information and conservative priors for the solar and average source peculiar motions, we estimate the distance to the Galactic center, Ro, to be 8.34 +/- 0.16 kpc, a circular rotation speed at the Sun, To, to be 240 +/- 8 km/s, and a rotation curve that is nearly flat (a slope of -0.2 +/- 0.4 km/s/kpc) between Galactocentric radii of 5 and 16 kpc. Assuming a "universal" spiral galaxy form for the rotation curve, we estimate the thin disk scale length to be 2.44 +/- 0.16 kpc. The parameters Ro and To are not highly correlated and are relatively insensitive to different forms of the rotation curve. Adopting a theoretically motivated prior that high-mass star forming regions are in nearly circular Galactic orbits, we estimate a global solar motion component in the direction of Galactic rotation, Vsun = 14.6 +/- 5.0 km/s. While To and Vsun are significantly correlated, the sum of these parameters is well constrained, To + Vsun = 255.2 +/- 5.1 km/s, as is the angular speed of the Sun in its orbit about the Galactic center, (To + Vsun)/Ro = 30.57 +/- 0.43 km/s/kpc. These parameters improve the accuracy of estimates of the accelerations of the Sun and the Hulse-Taylor binary pulsar in their Galactic orbits, significantly reducing the uncertainty in tests of gravitational radiation predicted by general relativity.Comment: 38 pages, 6 tables, 6 figures; v2 fixed typos and updated pulsar section; v3 replaced fig 2 (wrong file