The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves

We present optical and near-infrared (NIR) photometry and spectroscopy as well as modelling of the lightcurves of the Type IIb supernova (SN) 2011dh. Our extensive dataset, for which we present the observations obtained after day 100, spans two years, and complemented with Spitzer mid-infrared (MIR) data, we use it to build an optical-to-MIR bolometric lightcurve between days 3 and 732. To model the bolometric lightcurve before day 400 we use a grid of hydrodynamical SN models, which allows us to determine the errors in the derived quantities, and a bolometric correction determined with steady-state non-local thermodynamic equilibrium (NLTE) modelling. Using this method we find a helium core mass of 3.1^+0.7<inf>-0.4</inf> M<inf>⊙</inf> for SN 2011dh, consistent within error bars with previous results obtained using the bolometric lightcurve before day 80. We compute bolometric and broad-band lightcurves between days 100 and 500 from spectral steady-state NLTE models, presented and discussed in a companion paper. The preferred 12 M<inf>⊙</inf> (initial mass) model, previously found to agree well with the observed spectra, shows a good overall agreement with the observed lightcurves, although some discrepancies exist. Time-dependent NLTE modelling shows that after day ∼600 a steady-state assumption is no longer valid. The radioactive energy deposition in this phase is likely dominated by the positrons emitted in the decay of ⁵⁶Co, but seems insufficient to reproduce the lightcurves, and what energy source is dominating the emitted flux is unclear. We find an excess in the K and the MIR bands developing between days 100 and 250, during which an increase in the optical decline rate is also observed. A local origin of the excess is suggested by the depth of the He I 20 581 Å absorption. Steady-state NLTE models with a modest dust opacity in the core (τ = 0.44), turned on during this period, reproduce the observed behaviour, but an additional excess in the Spitzer 4.5 μm band remains. Carbon-monoxide (CO) first-overtone band emission is detected at day 206, and possibly at day 89, and assuming the additional excess to bedominated by CO fundamental band emission, we find fundamental to first-overtone band ratios considerably higher than observed in SN 1987A. The profiles of the [O i] 6300 Å and Mg i] 4571 Å lines show a remarkable similarity, suggesting that these lines originate from a common nuclear burning zone (O/Ne/Mg), and using small scale fluctuations in the line profiles we estimate a filling factor of ≲ 0.07 for the emitting material. This paper concludes our extensive observational and modelling work on SN 2011dh. The results from hydrodynamical modelling, steady-state NLTE modelling, and stellar evolutionary progenitor analysis are all consistent, and suggest an initial mass of ∼12 M<inf>⊙</inf> for the progenitor.

On the triple peaks of SNHunt248 in NGC 5806

We present our findings on a supernova (SN) impostor, SNHunt248, based on optical and near-IR data spanning ~15 yr before discovery, to ~1 yr post-discovery. The light curve displays three distinct peaks, the brightest of which is at MR ~ −15.0 mag. The post-discovery evolution is consistent with the ejecta from the outburst interacting with two distinct regions of circumstellar material. The 0.5–2.2 μm spectral energy distribution at −740 d is well-matched by a single 6700 K blackbody with log (L/L⊙) ~ 6.1. This temperature and luminosity support previous suggestions of a yellow hypergiant progenitor; however, we find it to be brighter than the brightest and most massive Galactic late-F to early-G spectral type hypergiants. Overall the historical light curve displays variability of up to ~ ± 1 mag. At current epochs (~1 yr post-outburst), the absolute magnitude (MR ~ − 9 mag) is just below the faintest observed historical absolute magnitude ~10 yr before discovery.

Locations of peculiar supernovae as a diagnostic of their origins

We put constraints on the properties of the progenitors of peculiar calcium-rich transients using the distribution of locations within their host galaxies. We confirm that this class of transients do not follow the galaxy stellar mass profile and are more likely to be found in remote locations of their apparent hosts. We test the hypothesis that these transients are from low-metallicity progenitors by comparing their spatial distributions with the predictions of self-consistent cosmological simulations that include star formation and chemical enrichment. We find that while metal-poor stars and our transient sample show a consistent preference for large offsets, metallicity alone cannot explain the extreme cases. Invoking a lower age limit on the progenitor helps to improve the match, indicating these events may result from a very old metal-poor population. We also investigate the radial distribution of globular cluster systems, and show that they too are consistent with the class of calcium-rich transients. Because photometric upper limits exist for globular clusters for some members of the class, a production mechanism related to the dense environment of globular clusters is not favoured for the calcium-rich events. However, the methods developed in this paper may be used in the future to constrain the effects of low metallicity on radially distant core-collapse events or help establish a correlation with globular clusters for other classes of peculiar explosions.

Differential effect of long versus short wavelength light exposure on pupillary re-dilation in patients with outer retinal disease.

BACKGROUND: In patients with outer retinal degeneration, a differential pupil response to long wavelength (red) versus short wavelength (blue) light stimulation has been previously observed. The goal of this study was to quantify differences in the pupillary re-dilation following exposure to red versus blue light in patients with outer retinal disease and compare them with patients with optic neuropathy and with healthy subjects. DESIGN: Prospective comparative cohort study. PARTICIPANTS: Twenty-three patients with outer retinal disease, 13 patients with optic neuropathy and 14 normal subjects. METHODS: Subjects were tested using continuous red and blue light stimulation at three intensities (1, 10 and 100 cd/m2) for 13 s per intensity. Pupillary re-dilation dynamics following the brightest intensity was analysed and compared between the three groups. MAIN OUTCOME MEASURES: The parameters of pupil re-dilation used in this study were: time to recover 90% of baseline size; mean pupil size at early and late phases of re-dilation; and differential re-dilation time for blue versus red light. RESULTS: Patients with outer retinal disease showed a pupil that tended to stay smaller after light termination and thus had a longer time to recovery. The differential re-dilation time was significantly greater in patients with outer retinal disease (median = 28.0 s, P < 0.0001) compared with controls and patients with optic neuropathy. CONCLUSIONS: A differential response of pupil re-dilation following red versus blue light stimulation is present in patients with outer retinal disease but is not found in normal eyes or among patients with visual loss from optic neuropathy.

Why I am not a teacher: a self-study examining why I made the decision to exit the teaching profession /

A good teacher was once described as being like a candle; consuming itself to light the way for others (Author unknown). But as Knox (2005) says, far too many yoimg flames flicker out before they ever get the opportvmity to bum their brightest. This self-study explores the phenomenon of teacher attrition through the stories and lived experiences of one elementary teacher. I strive throughout this self-study to delve deeper into the significance of my story and lived experiences in order to enhance our understanding of why teachers exit the profession. As a result, the guiding question throughout the study is, "Why do teachers, particularly those who have only taught for a few years, leave the classrooms they worked so hard to enter?" Through the writing of a narrative entitled Sarah 's Story, I was able to identify and give voice to a story openly sharing the feelings of despair; disappointment, frustration and disillusionment. This study has identified areas of tension that lead to dissatisfaction, discontent, and teacher disillusionment. It confronts the issues of complexity, uncertainty, and conflict that are experienced in teaching. It discusses the puzzling, powerfiil and upsetting experiences, highlighting the importance of talk between all members of the education system.

Out of the darkness and into the light : a study of inauthentic and authentic speech

Introduction Man can be described as the being who shows himself in speech, and from birth to death is continually speaking. Communication is so close to us, so woven into our very being, that we have little understanding of the way it is constituted; for it is as hard to obtain distance from communication as it is to obtain distance from ourselves. All communication is not alike. There are two basic modesl of communication, the inauthentic and the authentic, between which there occurs a constant tension. It is in the inauthentic mode, points out Heidegger, that we find ourselves "proximately and for the most part"; 1. Being and Time, pg. 68 Dasein decides as to the way it will comport itself in taking up its task of having being as an issue for it. " •.• it~, in its very being 'choose' itself and win itself; it can also lose itself and never win itself or only "seem" to do so. But only in so far as it is essentially something which can be authentic--that is, something of its own--can it have lost itself and not yet won itself." 2. therefore Heidegger also terms it "everydayness".2 Caught up in the world of everydayness, our speaking covers over and conceals3 our rootedness in being, leaving us in the darkness of untruth. The image of darkness may be inferred from Heidegger's use of the image of "clearing,,4 to depict being as 2. ibid. pg. 69 "Dasein's average everydayness, however, is not to be taken as a mere 'aspect'. Here too, and even in the mode of inauthenticity, the structure of existentiality lies ~ priori and here too Dasein's being is an issue for it in a definite way; and Dasein comports itself towards it the mode of average everydayness, even if this is only the mode of fleeing in the face of it and forgetfulness thereof." 3. ibid. pg. 59 "covering over" and "concealing" are 1;yays Dasein tries to flee its task of having being as an issue for itself. " ••• This being can be covered up so extensively that it becomes forgotten and no question arises about it or its meaning ••• n How everyday speaking accomplishes this will be taken up in detail in the second chapter which explores Dasein's everyday speech. 4. ibid, pg. 171 lI ••• we have in mind nothing other than the Existential - ontological structure of this entity (Dasein), that it is in such a way as to be its 'there'. To say that it is -' illuminated' [tlerleuchtet"] means that as Being-in-theworld it is cleared [gelichtetJ in itself7 not through any other entity, but in such a way that it is itself the clearing. Only for an entity which is eXistentially cleared in this way does what is present-at-hand become accessible in the light or hidden in the dark •••• " 3 dis-coveredness and truth. Our first task will be to explore the nature of communication in general and then to explore each of the modes manifested in turn. The structure of the inauthentic mode of communication can be explored by asking the following questions: What is this speaking about? Who is it that is speaking and who is spoken to? Does this speaking show man in his speech? The authentic mode is distinguished by the rarity with which we encounter it; as the inauthentic conceals, so the authentic reveals our rootedness in being. Yet this rarity makes it difficult to delineate its elusive structure clearly. Its constituent elements can be brought into focus by asking the same questions of this mode that we previously asked of the inauthentic mode. Our initial response to the disclosure of the authentic mode is to attempt to abandon the inauthentic mode and leave the darkness behind dwelling only in the "lighted place". All through the ages, some men pushing this to extreme, have, upon uncovering their relatedness to being, experienced a deep longing to dwell in such a "place" of pure truth and oft times denigrated or attempted to exclude the everyday world. Such 4. flight is twice mistaken: first it atbempts to fix truth as unchanging and static and secondly, it opposes this to untruth which it seeks to abolish. This is both the wrong view of truth and the wrong view of untruth as Heidegger points out in The Origin of The-Work of Art: The Way-to-be of truth, i.e., of discoveredness, is under the sway of refusal. But this refusal is no lack or privation, as if truth could be simply discoveredness rid of all covers. If it could be that, it would no longer be itself . ••• Truth in its way-to-be is untruth.5 Pure light is not the nature of Being nor is pure unconcealedness possible for man. Failure to remember this is the failure to realize that communication destroys itself in such flight because it no longer maintains the contingency of its task, i.e., the dis-closedness of being. We are reminded of the strong attraction this flight from darkness held for Plato. Light, truth and Being are all beyond the darkness and have nothing to do with it. In Book VII of the R~public, Socrates' explanation of the Allegory of the Cave to Glaucon points to a decided preference men have for the "lighted place". 5. The Origin Of The Work Of Art, pg. 42 5. Come then, I said, and join me in this further thought, and do not be surprised that those who attained to this height are not willing to occupy themselves with the affairs of men, but their souls ever feel the upward urge and yearning for that sojourn above. For this, I take it, is likely if in this point too the likeliness of our image holds. 6 Despite the attraction to pure truth, human communication is more complex than putting down one mode of communication and picking up another. Due to the fact that we are always on the way, the title of my thesis will have to be amended: OUT OF THE DARKNESS AND INTO THE LIGHT--AGAIN AND AGAIN. It must be this way because this is what it means to be human. This is the point made by Mephisto to Faust in pointing out that man, standing between God and the devil, needs both darkness and light: Er findet sich in einem ewigen Gl~t Uns hat er in die Finsternis gebracht, Und euch taugt einzig Tag und Nacht. 7 6. Republic z (517 c & d) It should be noted however, that while the philosopherking must be compelled to return to the cave for purely political reasons, once he has taken adequate view of the "brightest region of being" he has the full truth and his return to darkness adds nothing to the truth. 7. Faust, pg. 188 6. This thesis proposes to examine the grounds that give rise to communication, uncovering the structure of its inauthentic and authentic modes and paying close attention to tpeir interrelationship and to their relationship to language as "the house of Being": language that both covers and opens up man's rootedness in Being, transforming him as he moves along his way, taking up his "ownmost task" of becoming who he is. roots. He is the being who shows himself inn that reflects his forgetfulness or remembrance of his rootedness in being. Man comes into an already existent world and is addressedl through things in the world which are c

Étude de la cinématique HI (21cm) et H-Alpha de la galaxie du Triangle (M33).

Latex a été utilisé pour la redaction de cette thèse.

MPJ express meets gadget: towards a java code for cosmological simulations

Gadget-2 is a massively parallel structure formation code for cosmological simulations. In this paper, we present a Java version of Gadget-2. We evaluated the performance of the Java version by running colliding galaxies simulation and found that it can achieve around 70% of C Gadget-2's performance.

Cooled infrared filters and dichroics for the James Webb Space Telescope Mid-Infrared Instrument

The cooled infrared filters and dichroic beam splitters manufactured for the Mid-Infrared Instrument are key optical components for the selection and isolation of wavelengths in the study of astrophysical properties of stars, galaxies, and other planetary objects. We describe the spectral design and manufacture of the precision cooled filter coatings for the spectrometer (7 K) and imager (9 K). Details of the design methods used to achieve the spectral requirements, selection of thin film materials, deposition technique, and testing are presented together with the optical layout of the instrument. (C) 2008 Optical Society of America.

The distribution of interplanetary dust between 0.96 and 1.04 au as inferred from impacts on the STEREO spacecraft observed by the heliospheric imagers

The distribution of dust in the ecliptic plane between 0.96 and 1.04 au has been inferred from impacts on the two Solar Terrestrial Relations Observatory (STEREO) spacecraft through observation of secondary particle trails and unexpected off-points in the heliospheric imager (HI) cameras. This study made use of analysis carried out by members of a distributed web-based citizen science project Solar Stormwatch. A comparison between observations of the brightest particle trails and a survey of fainter trails shows consistent distributions. While there is no obvious correlation between this distribution and the occurrence of individual meteor streams at Earth, there are some broad longitudinal features in these distributions that are also observed in sources of the sporadic meteor population. The different position of the HI instrument on the two STEREO spacecraft leads to each sampling different populations of dust particles. The asymmetry in the number of trails seen by each spacecraft and the fact that there are many more unexpected off-points in the HI-B than in HI-A indicates that the majority of impacts are coming from the apex direction. For impacts causing off-points in the HI-B camera, these dust particles are estimated to have masses in excess of 10−17 kg with radii exceeding 0.1 μm. For off-points observed in the HI-A images, which can only have been caused by particles travelling from the anti-apex direction, the distribution is consistent with that of secondary ‘storm’ trails observed by HI-B, providing evidence that these trails also result from impacts with primary particles from an anti-apex source. Investigating the mass distribution for the off-points of both HI-A and HI-B, it is apparent that the differential mass index of particles from the apex direction (causing off-points in HI-B) is consistently above 2. This indicates that the majority of the mass is within the smaller particles of this population. In contrast, the differential mass index of particles from the anti-apex direction (causing off-points in HI-A) is consistently below 2, indicating that the majority of the mass is to be found in larger particles of this distribution.

Discovery in IC10 of the farthest known symbiotic star

We report the discovery of the first known symbiotic star in IC10, a starburst galaxy belonging to the Local Group, at a distance of similar to 750 kpc. The symbiotic star was identified during a survey of emission-line objects. It shines at V = 24.62 +/- 0.04, V - R(C) = 2.77 +/- 0.05 and R(C) - I(C) = 2.39 +/- 0.02, and suffers from E(B-V) = 0.85 +/- 0.05 reddening. The spectrum of the cool component well matches that of solar neighbourhood M8III giants. The observed emission lines belong to Balmer series, [S II], [N II] and [O III]. They suggest a low electronic density, negligible optical depth effects and 35 000 < T(eff) < 90 000 K for the ionizing source. The spectrum of the new symbiotic star in IC10 is an almost perfect copy of that of Hen 2-147, a well-known Galactic symbiotic star and Mira.

Hydrodynamical simulations of Galactic fountains - I. Evolution of single fountains

The ejection of the gas out of the disc in late-type galaxies is related to star formation and is due mainly to Type II supernovae. In this paper, we studied in detail the development of the Galactic fountains in order to understand their dynamical evolution and their influence on the redistribution of the freshly delivered metals over the disc. To this aim, we performed a number of 3D hydrodynamical radiative cooling simulations of the gas in the Milky Way where the whole Galaxy structure, the Galactic differential rotation and the supernova explosions generated by a single OB association are considered. A typical fountain powered by 100 Type II supernovae may eject material up to similar to 2 kpc which than collapses back mostly in the form of dense, cold clouds and filaments. The majority of the gas lifted up by the fountains falls back on the disc remaining within a radial distance Delta R = 0.5 kpc from the place where the fountain originated. This localized circulation of disc gas does not influence the radial chemical gradients on large scale, as required by the chemical models of the Milky Way which reproduce the metallicity distribution without invoking large fluxes of metals. Simulations of multiple fountains fuelled by Type II supernovae of different OB associations will be presented in a companion paper.

The old metal-poor open cluster ESO 92-SC05: accreted from a dwarf galaxy ?

The study of old open clusters outside the solar circle can bring constraints on formation scenarios of the outer disc. In particular, accretion of dwarf galaxies has been proposed as a likely mechanism in the area. We use BVI photometry for determining fundamental parameters of the faint open cluster ESO 92-SC05. Colour-magnitude diagrams are compared with Padova isochrones, in order to derive age, reddening and distance. We derive a reddening E(B - V) = 0.17, and an old age of similar to 6.0 Gyr. It is one of the rare open clusters known to be older than 5 Gyr. A metallicity of Z similar to 0.004 or [M/H] similar to -0.7 is found. The rather low metallicity suggests that this cluster might be the result of an accretion episode of a dwarf galaxy.

Predicting spectral features in galaxy spectra from broad-band photometry

We explore the prospects of predicting emission-line features present in galaxy spectra given broad-band photometry alone. There is a general consent that colours, and spectral features, most notably the 4000 angstrom break, can predict many properties of galaxies, including star formation rates and hence they could infer some of the line properties. We argue that these techniques have great prospects in helping us understand line emission in extragalactic objects and might speed up future galaxy redshift surveys if they are to target emission-line objects only. We use two independent methods, Artificial Neural Networks (based on the ANNz code) and Locally Weighted Regression (LWR), to retrieve correlations present in the colour N-dimensional space and to predict the equivalent widths present in the corresponding spectra. We also investigate how well it is possible to separate galaxies with and without lines from broad-band photometry only. We find, unsurprisingly, that recombination lines can be well predicted by galaxy colours. However, among collisional lines some can and some cannot be predicted well from galaxy colours alone, without any further redshift information. We also use our techniques to estimate how much information contained in spectral diagnostic diagrams can be recovered from broad-band photometry alone. We find that it is possible to classify active galactic nuclei and star formation objects relatively well using colours only. We suggest that this technique could be used to considerably improve redshift surveys such as the upcoming Fibre Multi Object Spectrograph (FMOS) survey and the planned Wide Field Multi Object Spectrograph (WFMOS) survey.

The spiral structure of the Galaxy revealed by CS sources and evidence for the 4:1 resonance

We present a map of the spiral structure of the Galaxy, as traced by molecular carbon monosulphide (CS) emission associated with IRAS sources which are believed to be compact H II regions. The CS line velocities are used to determine the kinematic distances of the sources in order to investigate their distribution in the galactic plane. This allows us to use 870 objects to trace the arms, a number larger than that of previous studies based on classical H II regions. The distance ambiguity of the kinematic distances, when it exists, is solved by different procedures, including the latitude distribution and an analysis of the longitude-velocity diagram. The study of the spiral structure is complemented with other tracers: open clusters, Cepheids, methanol masers and H II regions. The well-defined spiral arms are seen to be confined inside the corotation radius, as is often the case in spiral galaxies. We identify a square-shaped sub-structure in the CS map with that predicted by stellar orbits at the 4:1 resonance (four epicycle oscillations in one turn around the galactic centre). The sub-structure is found at the expected radius, based on the known pattern rotation speed and epicycle frequency curve. An inner arm presents an end with strong inwards curvature and intense star formation that we tentatively associate with the region where this arm surrounds the extremity of the bar, as seen in many barred galaxies. Finally, a new arm with concave curvature is found in the Sagitta to Cepheus region of the sky. The observed arms are interpreted in terms of perturbations similar to grooves in the gravitational potential of the disc, produced by crowding of stellar orbits.