Three-Dimensional Bar Structure and Disc/Bulge Secular Evolution

Kn-band imaging of a sample of 30 edge-on spiral galaxies with a boxy or peanut-shaped (B/PS) bulge is discussed. Galaxies with a B/PS bulge tend to have a more complex morphology than galaxies with other bulge types, unsharp-masked images revealing structures that trace the major orbit families of three-dimensional bars. Their surface brightness profiles are also more complex, typically containing 3 or more clearly separated regions, including a shallow or flat intermediate region (Freeman Type II profiles), suggestive of bar-driven transfer of angular momentum and radial redistribution of material. The data also suggest abrupt variations of the discs' scaleheights, as expected from the vertical resonances and instabilities present in barred discs but contrary to conventional wisdom. Counter to the standard `bulge + disc' model, we thus propose that galaxies with a B/PS bulge are composed of a thin concentrated disc (a disc-like bulge) contained within a partially thick bar (the B/PS bulge), itself contained within a thin outer disc. The inner disc most likely formed through bar-driven processes while the thick bar arises from buckling instabilities. Both are strongly coupled dynamically and are formed mostly of the same (disc) material.Comment: 6 pages, including 1 figure. To appear in "Island Universes: Structure and Evolution of Disk Galaxies", ed. R. de Jong (Springer: Dordrecht

LINC00507 Is Specifically Expressed in the Primate Cortex and Has Age-Dependent Expression Patterns

Over the past decade, there has been an increase in the appreciation of the role of non-coding RNA in the development of organism phenotype. It is possible to divide the non-coding elements of the transcriptome into three categories: short non-coding RNAs, circular RNAs and long non-coding RNAs. Long non-coding RNAs are those transcripts that are greater than 200 nts in length and lack any significant open reading frames that produce proteins greater then 100 amino acids. Long intervening non-coding RNAs (lincRNAs) are a subclass of long non-coding RNAs. In contrast to protein coding RNAs, lincRNAs are expressed in a more tissue- and species-specific manner. In particular, many lincRNAs are only conserved amongst higher primates. This coupled with the propensity of many lincRNAs to be expressed in the brain, suggests that they are in fact one of the major drivers of organism complexity. We analysed 39 lincRNAs that are expressed in the frontal cortex and identified LINC00507 as being expressed in a cortex-specific manner in non-human primates and humans. The expression patterns of LINC00507 appear to be age-dependent, suggesting it may be involved in brain development of higher primates. Moreover, the analysis of LINC00507 potential to bind ribosomes revealed that this previously identified non-coding transcript may harbour a micropeptide

Comparing peanut-shaped `bulges' to N-body simulations and orbital calculations

We present a near-infrared K_n-band photometric study of edge-on galaxies with a box/peanut-shaped `bulge'. The morphology of the galaxies is analysed using unsharp masking and fits to the vertical surface brightness profiles, and the results are compared to N-body simulations and orbital calculations of barred galaxies. Both theoretical approaches reproduce the main structures observed.Comment: 4 pages, 5 figures, to appear in the proceedings of "The Evoution of Galaxies. III. From simple approaches to self-consistent models" (Kiel, July 2002), G. Hensler et al. (eds.

Why Buckling Stellar Bars Weaken in Disk Galaxies

Young stellar bars in disk galaxies experience a vertical buckling instability which terminates their growth and thickens them, resulting in a characteristic peanut/boxy shape when viewed edge on. Using N-body simulations of galactic disks embedded in live halos, we have analyzed the bar structure throughout this instability and found that the outer third of the bar dissolves completely while the inner part (within the vertical inner Lindblad resonance) becomes less oval. The bar acquires the frequently observed peanut/boxy-shaped isophotes. We also find that the bar buckling is responsible for a mass injection above the plane, which is subsequently trapped by specific 3-D families of periodic orbits of particular shapes explaining the observed isophotes, in line with previous work. Using a 3-D orbit analysis and surfaces of sections, we infer that the outer part of the bar is dissolved by a rapidly widening stochastic region around its corotation radius -- a process related to the bar growth. This leads to a dramatic decrease in the bar size, decrease in the overall bar strength and a mild increase in its pattern speed, but is not expected to lead to a complete bar dissolution. The buckling instability appears primarily responsible for shortening the secular diffusion timescale to a dynamical one when building the boxy isophotes. The sufficiently long timescale of described evolution, ~1 Gyr, can affect the observed bar fraction in local universe and at higher redshifts, both through reduced bar strength and the absence of dust offset lanes in the bar.Comment: 7 pages, 4 figures, ApJ Letters, in pres

Neonatal screening for congenital hypothyroidism in an Italian Centre: a 5-years real-life retrospective study

Introduction: Congenital hypothyroidism is an endocrine disease with a significant incidence in the general population (1:2000–1:3000 newborns in Italy) and a different geographical distribution, partially explained by endemic iodine deficiency, genetic traits and autoimmune thyroid diseases. Objectives: Aims of this study are: to evaluate the incidence of positive neonatal blood spot screening for CH in western Sicily, identified by the screening centre of the Children Hospital “G. Di Cristina”, ARNAS, Palermo; to evaluate the impact of a lower TSH cutoff in the neonatal blood spot screening for CH. Materials and methods: The TSH threshold of the neonatal screening was established as ≥6 mU/L of whole blood. We analysed the screening centre data in the period January 2013–April 2018, for a total number of 85.373 babies (45.7% males; 54.3% females). Results: 4.082 Babies (4.8%) required a second screening. Among these, 372 (0.44%) were out of range. The diagnosis of congenital hypothyroidism (CH) was confirmed in 182 babies (0.21%). 77/372 newborns (20.7%) with confirmed high TSH levels showed whole blood TSH levels ≥6 - < 7 mU/L. In synthesis, 48.9% of the out of range re-testing had a confirmed diagnosis of CH. Conclusion: The reduction of TSH cutoff to 6 mU/L allowed to identify 77/372 neonates (20.7%) with confirmed out of range TSH, otherwise not recruited by the previously employed TSH cutoff

K-Band Observations of Boxy Bulges. I. Morphology and Surface Brightness Profiles

Kn-band images, unsharp-masked images, as well as major-axis and vertically- summed surface brightness profiles are presented for 30 edge-on spiral galaxies, most with a boxy or peanut-shaped (B/PS) bulge. Such galaxies have more complex morphologies than galaxies of other bulge types, more often showing (off-)centered X structures, secondary major-axis maxima and spiral-like structures. Those features are also observed in N-body simulations of barred discs and may trace the main bar orbit families. The surface brightness profiles of galaxies with a B/PS bulge are also more complex, with typically 3 or more clearly separated regions, including a flat intermediate region (Freeman Type II profiles). Those radial breaks offer evidence for bar-driven transfer of angular momentum and radial redistribution of material. The profiles also suggest a rapid variation of the scaleheight of the disc material, contrary to conventional wisdom but again as expected from vertical resonances and instabilities in barred discs. The steep inner region of the surface brightness profiles is often shorter than the isophotally thick part of the galaxies, itself always shorter than the flat region of the profiles. Contrary to the standard `bulge + disc' model, we thus propose that galaxies with a B/PS bulge are composed of a thin concentrated disc (a disc-like bulge) contained within a partially thick bar (the B/PS bulge) and a thin outer disc. The inner disc likely formed secularly through bar-driven processes and is responsible for the steep inner region of the surface brightness profiles, while the bar is responsible for the flat region and the thick complex morphological structures observed. Those components are strongly coupled dynamically and are formed mostly of the same (disc) material. [Abridged]Comment: 23 pages, 34 figures. Accepted for publication in MNRAS. A version with full resolution figures is available at http://www-astro.physics.ox.ac.uk/~bureau/pub_list.htm

LINC00507 Is Specifically Expressed in the Primate Cortex and Has Age-Dependent Expression Patterns

General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. Abstract Over the past decade, there has been an increase in the appreciation of the role of non-coding RNA in the development of organism phenotype. It is possible to divide the non-coding elements of the transcriptome into three categories: short non-coding RNAs, circular RNAs and long non-coding RNAs. Long non-coding RNAs are those transcripts that are greater than 200 nts in length and lack any significant open reading frames that produce proteins greater then 100 amino acids. Long intervening non-coding RNAs (lincRNAs) are a subclass of long non-coding RNAs. In contrast to protein coding RNAs, lincRNAs are expressed in a more tissue-and species-specific manner. In particular, many lincRNAs are only conserved amongst higher primates. This coupled with the propensity of many lincRNAs to be expressed in the brain, suggests that they are in fact one of the major drivers of organism complexity. We analysed 39 lincRNAs that are expressed in the frontal cortex and identified LINC00507 as being expressed in a cortex-specific manner in non-human primates and humans. The expression patterns of LINC00507 appear to be age-dependent, suggesting it may be involved in brain development of higher primates. Moreover, the analysis of LINC00507 potential to bind ribosomes revealed that this previously identified non-coding transcript may harbour a micropeptide

Bar Diagnostics in Edge-On Spiral Galaxies. III. N-Body Simulations of Disks

Present in over 45% of local spirals, boxy and peanut-shaped bulges are generally interpreted as edge-on bars and may represent a key phase in the evolution of bulges. Aiming to test such claims, the kinematic properties of self-consistent 3D N-body simulations of bar-unstable disks are studied. Using Gauss-Hermite polynomials to describe the stellar kinematics, a number of characteristic bar signatures are identified in edge-on disks: 1) a major-axis light profile with a quasi-exponential central peak and a plateau at moderate radii (Freeman Type II profile); 2) a ``double-hump'' rotation curve; 3) a sometime flat central velocity dispersion peak with a plateau at moderate radii and occasional local central minimum and secondary peak; 4) an h3-V correlation over the projected bar length. All those kinematic features are spatially correlated and can easily be understood from the orbital structure of barred disks. They thus provide a reliable and easy-to-use tool to identify edge-on bars. Interestingly, they are all produced without dissipation and are increasingly realized to be common in spirals, lending support to bar-driven evolution scenarios for bulge formation. So called ``figure-of-eight'' position-velocity diagrams are never observed, as expected for realistic orbital configurations. Although not uniquely related to triaxiality, line-of-sight velocity distributions with a high velocity tail (i.e. an h3-V correlation) appear as particularly promising tracers of bars. The stellar kinematic features identified grow in strength as the bar evolves and vary little for small inclination variations. Many can be used to trace the bar length. Comparisons with observations are encouraging and support the view that boxy and peanut-shaped bulges are simply thick bars viewed edge-on.Comment: 32 pages, 4 figures, AASTeX preprint. Revised following referees' comments. Now accepted for publication in The Astrophysical Journal. We strongly suggest you download the version with full resolution figures at http://www.astro.columbia.edu/~bureau/Publications/Nbody_ApJ04.ps.g