Star Formation Density and Halpha Luminosity Function of an Emission Line Selected Galaxy Sample at z ~ 0.24

We use narrowband imaging (FWHM = 70 A) to select a sample of emission line galaxies between 0.20 <~ z <~ 1.22 in two fields covering 0.5 sq. deg. We use spectroscopic follow-up to select a sub-sample of Halpha emitting galaxies at z ~ 0.24 and determine the Halpha luminosity function and star formation density at z ~ 0.24 for both of our fields. Corrections are made for imaging and spectroscopic incompleteness, extinction and interloper contamination on the basis of the spectroscopic data. When compared to each other, we find the field samples differ by \Delta \alpha = 0.2 in faint end slope and \Delta \log [ L* (ergs/s) ] = 0.2 in luminosity. In the context of other recent surveys, our sample has comparable faint end slope, but a fainter L* turn-over. We conclude that systematic uncertainties and differences in selection criteria remain the dominant sources of uncertainty between Halpha luminosity functions at this redshift. We also investigate average star formation rates as a function of local environment and find typical values consistent with the field densities that we probe, in agreement with previous results. However, we find tentative evidence for an increase in star formation rate with respect to the local density of star forming galaxies, consistent with the scenario that galaxy-galaxy interactions are triggers for bursts of star formation.Comment: Accepted for publication in MNRAS. The paper contains 14 figures and 7 table

The universality of poetry in Aristotle’s Poetics

This paper considers three questions arising out of Aristotle's statement that poetry is concerned with the universal. First, what does it mean? Secondly, what constraints does it impose on the construction of (in particular) tragic plots? This question is considered with special reference to the possible role of chance in tragedy. Thirdly, why is poetry concerned with the universal— that is, why is poetry such that these constraints are appropriate? In chapter 9 of the Poetics Aristotle states that poetry is concerned with the universal. In this paper I shall consider three questions arising out of this statement. First, what does it mean? Secondly, what constraints does it impose on the construction of (in particular) tragic plots? I shall consider this question with special reference to the possible role of chance in tragedy. Thirdly, why is poetry concerned with the universal—that is, why is poetry such that these constraints are appropriate

Regional variability in the trophic requirements of shelf sea fisheries in the Northeast Atlantic, 1973-2000

Hydrographic, plankton, benthos, fisheries landings, and fish diet data from shelf sea areas in the Northeast Atlantic have been combined into an analysis of the foodweb structure and secondary production requirements of regional fisheries. Fish landings from the Baltic and North Sea are shown to be taken from a lower trophic level and are shown to be overall more planktivorous than those from shelf edge regions. The secondary production required per unit of landed fish from the North Sea was approximately half that for landings from the southwest approaches to the UK, referred to as the Celtic Seas, where zooplankton production accounted for only a small fraction of the secondary production demands of the fisheries. In the North Sea, variability in zooplankton production seems to have exerted a bottom-up effect on fish production, which in turn has exerted a top-down effect on the benthos. Conversely, Celtic Seas benthos production has been a bottom-up driver of fish production, which seems to have been independent of variability in plankton production.Thus, climate and fishing pressures can be expected to influence these regional fisheries in very different ways. Overall, the results indicate very strong spatial patterns in the fish foodweb structure and function, which will be important considerations in the establishment of regional management plans for fisheries

Towards human technology symbiosis in the haptic mode

Search and rescue operations are often undertaken in dark and noisy environments in which rescue teams must rely on haptic feedback for exploration and safe exit. However, little attention has been paid specifically to haptic sensitivity in such contexts or to the possibility of enhancing communicational proficiency in the haptic mode as a life-preserving measure. Here we discuss the design of a haptic guide robot, inspired by careful study of the communication between blind person and guide dog. In the case of this partnership, the development of a symbiotic relationship between person and dog, based on mutual trust and confidence, is a prerequisite for successful task performance. We argue that a human-technology symbiosis is equally necessary and possible in the case of the robot guide. But this is dependent on the robot becoming 'transparent technology' in Andy Clark's sense. We report on initial haptic mode experiments in which a person uses a simple mobile mechanical device (a metal disk fixed with a rigid handle) to explore the immediate environment. These experiments demonstrate the extreme sensitivity and trainability of haptic communication and the speed with which users develop and refine their haptic proficiencies in using the device, permitting reliable and accurate discrimination between objects of different weights. We argue that such trials show the transformation of the mobile device into a transparent information appliance and the beginnings of the development of a symbiotic relationship between device and human user. We discuss how these initial explorations may shed light on the more general question of how a human mind, on being exposed to an unknown environment, may enter into collaboration with an external information source in order to learn about, and navigate, that environment

Environments and Morphologies of Red Sequence Galaxies with Residual Star Formation in Massive Clusters

We present a photometric investigation into recent star formation in galaxy clusters at z ~ 0.1. We use spectral energy distribution templates to quantify recent star formation in large X-ray selected clusters from the LARCS survey using matched GALEX NUV photometry. These clusters all have signs of red sequence galaxy recent star formation (as indicated by blue NUV-R colour), regardless of cluster morphology and size. A trend in environment is found for these galaxies, such that they prefer to occupy low density, high cluster radius environments. The morphology of these UV bright galaxies suggests that they are in fact red spirals, which we confirm with light curves and Galaxy Zoo voting percentages as morphological proxies. These UV bright galaxies are therefore seen to be either truncated spiral galaxies, caught by ram pressure in falling into the cluster, or high mass spirals, with the photometry dominated by the older stellar population.Comment: Accepted for publication in MNRAS, 11 pages, 11 figure

Evidence for HI replenishment in massive galaxies through gas accretion from the cosmic web

We examine the H i -to-stellar mass ratio (H i fraction) for galaxies near filament backbones within the nearby Universe (d &lt; 181 Mpc). This work uses the 6 degree Field Galaxy Survey (6dFGS) and the Discrete Persistent Structures Extractor (DisPerSE) to define the filamentary structure of the local cosmic web. H i spectral stacking of H i Parkes All Sky Survey (HIPASS) observations yield the H i fraction for filament galaxies and a field control sample. The H i fraction is measured for different stellar masses and 5th nearest neighbour projected densities (Σ5) to disentangle what influences cold gas in galaxies. For galaxies with stellar masses log(M⋆) ≤ 11 M⊙ in projected densities 0 ≤ Σ5 &lt; 3 galaxies Mpc−2, all H i fractions of galaxies near filaments are statistically indistinguishable from the control sample. Galaxies with stellar masses log(M⋆) ≥ 11 M⊙ have a systematically higher H i fraction near filaments than the control sample. The greatest difference is 0.75 dex, which is 5.5σ difference at mean projected densities of 1.45 galaxies Mpc−2. We suggest that this is evidence for massive galaxies accreting cold gas from the intra-filament medium which can replenish some H i gas. This supports cold mode accretion where filament galaxies with a large gravitational potential can draw gas from the large scale structure

The Clustering Of Galaxies Around Radio-Loud AGNs

We examine the hypothesis that mergers and close encounters between galaxies can fuel AGNs by increasing the rate at which gas accretes towards the central black hole. We compare the clustering of galaxies around radio-loud AGNs with the clustering around a population of radio-quiet galaxies with similar masses, colors and luminosities. Our catalog contains 2178 elliptical radio galaxies with flux densities greater than 2.8 mJy at 1.4 GHz from the 6dFGS survey. We find that radio AGNs with more than 200 times the median radio power have, on average, more close (r<160 kpc) companions than their radio-quiet counterparts, suggestive that mergers play a role in forming the most powerful radio galaxies. For ellipticals of fixed stellar mass, the radio power is not a function of large-scale environment nor halo mass, consistent with the radio powers of ellipticals varying by orders of magnitude over billions of years.Comment: 12 pages, 6 figure