Dwarf irregular galaxies with extended HI gas disks: Suppression of small-scale spiral structure by dark matter halo

Dwarf irregular galaxies with extended HI disk distributions, such as DDO 154, allow measurement of rotation curves, hence deduction of dark matter halo properties to large radial distances, up to several times the optical radius. These galaxies contain a huge reservoir of dark matter halo, which dominates over most of disk. We study the effect of the dark matter halo on small-scale spiral features by carrying out the local, non-axisymmetric perturbation analysis in the disks of five such late-type, gas-rich dwarf irregular galaxies, namely, DDO 154, NGC 3741, DDO 43, NGC 2366, and DDO 168 which host a dense and compact dark matter halo. We show that when the gas disk is treated alone, it allows a finite swing amplification; which would result in small-scale spiral structure in the outer gas disk, but the addition of dark matter halo in the analysis results in a higher Toomre Q parameter which prevents the amplification almost completely. This trend is also seen to be true in regions inside the optical radius. This implies absence of strong small-scale spiral arms in these galaxies, which is in agreement with observations. Hence despite being gas-rich, and in fact having gas as the main baryonic component, these galaxies cannot support small-scale spiral structure which would otherwise have been expected in normal gas-rich galaxies.Comment: 30 pages, 6 figures, 1 table, accepted for publication in New Astronom

Suppression of gravitational instabilities by dominant dark matter halo in low surface brightness galaxies

The low surface brightness galaxies are gas-rich and yet have a low star formation rate, this is a well-known puzzle. The spiral features in these galaxies are weak and difficult to trace, although this aspect has not been studied much. These galaxies are known to be dominated by the dark matter halo from the innermost regions. Here we do a stability analysis for the galactic disc of UGC 7321, a low surface brightness, superthin galaxy, for which the various observational input parameters are available. We show that the disc is stable against local, linear axisymmetric and non-axisymmetric perturbations. The Toomre Q parameter values are found to be large (>> 1) mainly due to the low disc surface density and the high rotation velocity resulting due to the dominant dark matter halo, which could explain the observed low star formation rate. For the stars-alone case, the disc shows finite swing amplification but the addition of dark matter halo suppresses that amplification almost completely. Even the inclusion of the low-dispersion gas which constitutes a high disc mass fraction does not help in causing swing amplification. This can explain why these galaxies do not show strong spiral features. Thus the dynamical effect of a halo that is dominant from inner regions can naturally explain why star formation and spiral features are largely suppressed in low surface brightness galaxies, making these different from the high surface brightness galaxies.Comment: 7 pages, 2 figures, 1 table, accepted for publication in MNRA

Role of gas in supporting grand spiral structure

The density wave theory for the grand-design two-armed spiral pattern in galaxies is successful in explaining several observed features. However, the long-term persistence of this spiral structure is a serious problem since the group transport would destroy it within about a billion years as shown in a classic paper by Toomre. In this paper we include the low velocity dispersion component, namely gas, on an equal footing with stars in the formulation of the density wave theory, and obtain the dispersion relation for this coupled system. We show that the inclusion of gas makes the group transport slower by a factor of few, thus allowing the pattern to persist longer - for several billion years. Though still less than the Hubble time, this helps in making the spiral structure more long-lived. Further we show that addition of gas is essential to get a stable wave for the observed pattern speed for the Galaxy, which otherwise is not possible for a one-component stellar disc.Comment: 6 pages, 3 figures, 1 table, accepted for publication in MNRA

Effect of finite disk-thickness on swing amplification of non-axisymmetric perturbations in a sheared galactic disk

A typical galactic disk is observed to have a finite thickness. Here, we present the study of the physical effect of introduction of finite thickness on the generation of small-scale spiral arms by swing amplification in a differentially rotating galactic disk. The galactic disk is modelled first as a one-fluid system, and then as a gravitationally-coupled two-fluid (stars and gas) system where each fluid is taken as isothermal, and corotating with each other. We derived the equations governing the evolution of growth of the non-axisymmetric perturbations in a sheared frame of reference while incorporating the effect of finite thickness of a galactic disk. We found that the finite thickness of a galactic disk has a generic trend of suppressing the growth of the non-axisymmetric perturbations via swing amplification. Moreover, even the observed range of disk-thickness values (~ 300-500 pc) can lead to a complete suppression of swing amplification for Q ~ 1.7, whereas for an infinitesimally-thin disk, the corresponding critical value is Q ~ 2. For a two-fluid (stars and gas) system, the net amplification is shown to be set by the mutual interplay of the effect of interstellar gas in promoting the spiral features and the effect of finite thickness in preventing the spiral arms. The coexistence of these two opposite effects is shown to be capable of giving rise to diverse and complex dynamical behaviour.Comment: 13 pages, 8 figures, accepted for publication in A&

Looking for a needle in a haystack : how to measure the length of a stellar bar?

One of the challenges related to stellar bars is to determine accurately the length of the bar in a disc galaxy. In past literature, a wide variety of methods has been employed to measure the extent of a bar. However, a systematic study on determining the robustness and accuracy of different bar length estimators is still beyond our grasp. Here, we investigate the accuracy and the correlation (if any) between different bar length measurement methods while using an $N$-body model of a barred galaxy where the bar evolves self-consistently in presence of a live dark matter halo. We investigate the temporal evolution of the bar length, using different estimators (involving isophotal analysis of de-projected surface brightness distribution and Fourier decomposition of surface density), and study their robustness and accuracy. Further attempts have been made towards determining correlation between any two of these bar length estimators used here. In presence of spirals, the bar length estimators which only consider the amplitudes of different Fourier moments (and do not take into account the phase-angle of $m=2$ Fourier moment), systematically overestimate the length of the bar. The strength dark-gaps (produced by bars) correlates strongly with the bar length in early rapid growth phase, and is only weakly anti-correlated during subsequent quiescent phase of bar evolution. However, the location of dark-gaps correlates only weakly with the bar length, hence can not be used as a robust proxy for determining the bar length. In addition, the bar length estimators, obtained using isophotal analysis of de-projected surface brightness distribution, systematically overestimate the bar length. The implications of bar length over(under)estimation in the context of determining fast/slow bars are further discussed.Comment: 12 pages, 10 figures (including appendix), comments are welcome

Trinuclear heterometallic CuII-MnII complexes of a salen type Schiff base ligand: anion dependent variation of phenoxido bridging angles and magnetic coupling

Five new trinuclear heterometallic CuII-MnII complexes [(CuL)2Mn(O2CPh)2] (1), [(CuL)2Mn(N3)2] (2), [(CuL)2Mn(NCO)2] (3), [(CuL)2Mn(NO3)2] (4) and [(CuL)2Mn(Sal)2]∙CH2Cl2 (5) have been synthesized with the di-Schiff base ligand H2L (where, H2L= N,N'-bis(salicylidene)-1,3-propanediamine and Sal= salicylate). These complexes with different anionic co-ligands have been synthesized to attain a large variation in phenoxido bridging angles and to investigate its consequence on magnetic properties. Single crystal X-ray diffraction analyses reveal that complexes 1, 2, 4 and 5 are linear, whereas 3 has an angular geometry. Variable temperature magnetic susceptibility measurements suggest that all five complexes possess an overall antiferromagnetic interaction between CuII and MnII ions, which results in a final ferrimagnetic ground state with spin 3/2 in the CuII-MnII-CuII trinuclear structure. The weakest antiferromagnetic interaction (JCu-Mn= -7.0 cm-1) is observed for 2 having the lowest value of the Cu-O-Mn angle (92.0°), while the strongest antiferromagnetic interaction (JCu-Mn= -26.5 cm-1) is observed for 3 having the largest Cu-O-Mn angle (101.4°). Complexes 1, 4 and 5 show an average Cu-O-Mn angles of 98.2°, 97.6° and 97.7°, respectively, that lead to intermediate antiferromagnetic interactions (JCu-Mn = -9.6, -9.7, -9.3 cm-1 respectively)

Quantifying the influence of bars on action-based dynamical modelling of disc galaxies

Action-based dynamical modelling, using stars as dynamical tracers, is an excellent diagnostic to estimate the underlying axisymmetric matter distribution of the Milky Way. However, the Milky Way's bar causes non-axisymmetric resonance features in the stellar disc. Using Roadmapping (an action-based dynamical modelling framework to estimate the gravitational potential and the stellar distribution function), we systematically quantify the robustness of action-based modelling in the presence of a bar. We construct a set of test-particle simulations of barred galaxies (with varying bar properties), and apply Roadmapping to different survey volumes (with varying azimuthal position, size) drawn from these barred models. For realistic bar parameters, the global potential parameters are still recovered to within ${\sim \! 1 \! - \! 20}$ percent. However, with increasing bar strength, the best-fit values of the parameters progressively deviate from their true values. This happens due to a combination of radial heating, radial migration, and resonance overlap phenomena in our bar models. Furthermore, the azimuthal location and the size of the survey volumes play important roles in the successful recovery of the parameters. Survey volumes along the bar major axis produce larger (relative) errors in the best-fit parameter values. In addition, the potential parameters are better recovered for survey volumes with larger spatial coverage. As the Sun is located just ${\sim \! 28 \! - \! 33}$ degrees behind the bar's major axis, an estimate for the bar-induced systematic bias -- as provided by this study -- is therefore crucial for future modelling attempts of the Milky Way.Comment: 18 pages, 10 figures, 2 tables, comments are welcom

Bars and boxy/peanut bulges in thin and thick discs. II. Can bars form in hot thick discs?

The Milky Way as well as a majority of external galaxies possess a thick disc. However, the dynamical role of the (geometrically) thick disc on the bar formation and evolution is not fully understood. Here, we investigate the effect of thick discs in bar formation and evolution by means of a suite of N-body models of (kinematically cold) thin-(kinematically hot) thick discs. We systematically vary the mass fraction of the thick disc, the thin-to-thick disc scale length ratio as well as thick disc's scale height to examine the bar formation under diverse dynamical scenarios. Bars form almost always in our models, even in presence of a massive thick disc. The part of the bar constituted by the thick disc closely follows the overall growth and temporal evolution of the part of the bar constituted by the thin disc, only the part of the bar in the thick disc is weaker than the part of the bar in the thin disc. The formation of stronger bars is associated with a simultaneous larger loss of angular momentum and a larger radial heating. In addition, we demonstrate a preferential loss of angular momentum and a preferential radial heating of disc stars, along the azimuthal direction within the extent of the bar, in both thin and thick disc stars. For purely thick disc models (without any thin disc), the bar formation critically depends on the disc scale length and scale height. A larger scale length and/or a larger vertical scale height delays the bar formation time and/or suppresses the bar formation almost completely in thick-disc-only models. We find that the Ostriker-Peeble criterion predicts the bar instability scenarios in our models better than the Efstathiou-Lake-Negroponte criterion.Comment: 20 pages, 14 figures, 1 table (including appendix), accepted for publication in A&

A whole school approach to literacy intervention

This research project reports on the process of developing a whole school approach to literacy intervention in one multi-ethnic, designated disadvantaged primary school. The study describes how teachers worked collaboratively, using items from a resource package Successful Intervention K-3 Literacy, to critically reflect on their pedagogy in their efforts to better address the needs of those students in their classes who appeared to have difficulties with literacy learning. A modified action research method was used by the teachers to devise a context-specific school plan. Within the plan, they allocated time and resources to assist them as they shared and developed their knowledge and skills to deal with the social, cultural, emotional, linguistic and cognitive needs of the identified students. As a result, the teachers developed individual literacy intervention programs for children experiencing difficulties. The programs included all the stake holders and were devised to be used in the mainstream classrooms. In addition, in order to facilitate consistency and continuity of approach from year to year for students experiencing difficulty with literacy learning, the teachers planned a system to store and pass on students\u27 records. Of particular interest were the actions taken to explore understandings about literacy interventions, the changes in teacher perceptions, and the use of individual literacy intervention programs for children experiencing difficulties with literacy learning. As a consequence of their involvement in the project, the teachers developed an integrated literacy intervention policy and a school plan to guide future strategies for literacy intervention