The Unusually Luminous Extragalactic Nova SN 2010U

We present observations of the unusual optical transient SN 2010U, including spectra taken 1.03 days to 15.3 days after maximum light that identify it as a fast and luminous Fe II type nova. Our multi-band light curve traces the fast decline (t 2 = 3.5 ± 0.3 days) from maximum light (MV = -10.2 ± 0.1 mag), placing SN 2010U in the top 0.5% of the most luminous novae ever observed. We find typical ejecta velocities of ≈1100 km s-1 and that SN 2010U shares many spectral and photometric characteristics with two other fast and luminous Fe II type novae, including Nova LMC 1991 and M31N-2007-11d. For the extreme luminosity of this nova, the maximum magnitude versus rate of decline relationship indicates a massive white dwarf (WD) progenitor with a low pre-outburst accretion rate. However, this prediction is in conflict with emerging theories of nova populations, which predict that luminous novae from massive WDs should preferentially exhibit an alternate spectral type (He/N) near maximum light.

SN 2010ay is a Luminous and Broad-lined Type Ic Supernova within a Low-metallicity Host Galaxy

We report on our serendipitous pre-discovery detection and follow-up observations of the broad-lined Type Ic supernova (SN Ic) 2010ay at z = 0.067 imaged by the Pan-STARRS1 3π survey just ~4 days after explosion. The supernova (SN) had a peak luminosity, MR ≈ -20.2 mag, significantly more luminous than known GRB-SNe and one of the most luminous SNe Ib/c ever discovered. The absorption velocity of SN 2010ay is v Si ≈ 19 × 103 km s-1 at ~40 days after explosion, 2-5 times higher than other broad-lined SNe and similar to the GRB-SN 2010bh at comparable epochs. Moreover, the velocity declines ~2 times slower than other SNe Ic-BL and GRB-SNe. Assuming that the optical emission is powered by radioactive decay, the peak magnitude implies the synthesis of an unusually large mass of 56Ni, M Ni = 0.9 M ⊙. Applying scaling relations to the light curve, we estimate a total ejecta mass, M ej ≈ 4.7 M ⊙, and total kinetic energy, EK ≈ 11 × 1051 erg. The ratio of M Ni to M ej is ~2 times as large for SN 2010ay as typical GRB-SNe and may suggest an additional energy reservoir. The metallicity (log (O/H)PP04 + 12 = 8.19) of the explosion site within the host galaxy places SN 2010ay in the low-metallicity regime populated by GRB-SNe, and ~0.5(0.2) dex lower than that typically measured for the host environments of normal (broad-lined) SNe Ic. We constrain any gamma-ray emission with E γ ~ 1048 erg. We therefore rule out the association of a relativistic outflow like those that accompanied SN 1998bw and traditional long-duration gamma-ray bursts (GRBs), but we place less-stringent constraints on a weak afterglow like that seen from XRF 060218. If this SN did not harbor a GRB, these observations challenge the importance of progenitor metallicity for the production of relativistic ejecta and suggest that other parameters also play a key role.

Ultraluminous Supernovae as a New Probe of the Interstellar Medium in Distant Galaxies

We present the Pan-STARRS1 discovery and light curves, and follow-up MMT and Gemini spectroscopy of an ultraluminous supernova (ULSN; dubbed PS1-11bam) at a redshift of z = 1.566 with a peak brightness of M UV ≈ -22.3 mag. PS1-11bam is one of the highest redshift spectroscopically confirmed SNe known to date. The spectrum exhibits broad absorption features typical of previous ULSNe (e.g., C II, Si III), and strong and narrow Mg II and Fe II absorption lines from the interstellar medium (ISM) of the host galaxy, confirmed by an [O II]λ3727 emission line at the same redshift. The equivalent widths of the Fe II λ2600 and Mg II λ2803 lines are in the top quartile of the quasar intervening absorption system distribution, but are weaker than those of gamma-ray burst intrinsic absorbers (i.e., GRB host galaxies). We also detect the host galaxy in pre-explosion Pan-STARRS1 data and find that its UV spectral energy distribution is best fit with a young stellar population age of τ* ≈ 15-45 Myr and a stellar mass of M * ≈ (1.1-2.6) × 109 M ⊙ (for Z = 0.05-1 Z ⊙). The star formation rate inferred from the UV continuum and [O II]λ3727 emission line is ≈10 M ⊙ yr-1, higher than in previous ULSN hosts. PS1-11bam provides the first direct demonstration that ULSNe can serve as probes of the ISM in distant galaxies. The depth and red sensitivity of PS1 are uniquely suited to finding such events at cosmologically interesting redshifts (z ~ 1-2); the future combination of LSST and 30 m class telescopes promises to extend this technique to z ~ 4.

On the diversity of superluminous supernovae: ejected mass as the dominant factor

We assemble a sample of 24 hydrogen-poor superluminous supernovae(SLSNe). Parameterizing the light-curve shape through rise and declinetime-scales shows that the two are highly correlated. Magnetar-poweredmodels can reproduce the correlation, with the diversity in rise anddecline rates driven by the diffusion time-scale. Circumstellarinteraction models can exhibit a similar rise-decline relation, but onlyfor a narrow range of densities, which may be problematic for thesemodels. We find that SLSNe are approximately 3.5 mag brighter and havelight curves three times broader than SNe Ibc, but that the intrinsicshapes are similar. There are a number of SLSNe with particularly broadlight curves, possibly indicating two progenitor channels, butstatistical tests do not cleanly separate two populations. The generalspectral evolution is also presented. Velocities measured from Fe II aresimilar for SLSNe and SNe Ibc, suggesting that diffusion timedifferences are dominated by mass or opacity. Flat velocity evolution inmost SLSNe suggests a dense shell of ejecta. If opacities in SLSNe aresimilar to other SNe Ibc, the average ejected mass is higher by a factor2-3. Assuming κ = 0.1 cm2 g-1, we estimate amean (median) SLSN ejecta mass of 10 M⊙ (6M⊙), with a range of 3-30 M⊙. Doubling theassumed opacity brings the masses closer to normal SNe Ibc, but with ahigh-mass tail. The most probable mechanism for generating SLSNe seemsto be the core collapse of a very massive hydrogen-poor star, forming amillisecond magnetar.

A supernova distance to the anchor galaxy NGC 4258

The fortuitous occurrence of a type II-Plateau (IIP) supernova, SN 2014bc, in a galaxy for which distance estimates from a number of primary distance indicators are available provides a means with which to cross-calibrate the standardised candle method (SCM) for type IIP SNe. By applying calibrations from the literature we find distance estimates in line with the most precise measurement to NGC 4258 based on the Keplerian motion of masers (7:6 ± 0:23 Mpc), albeit with significant scatter. We provide an alternative local SCM calibration by only considering type IIP SNe that have occurred in galaxies for which a Cepheid distance estimate is available. We find a considerable reduction in scatter (σ<inf>I</inf> = 0:16 mag), but note that the current sample size is limited. Applying this calibration, we estimate a distance to NGC 4258 of 7:08 ± 0:86 Mpc.

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.

YSOVAR: Mid-infrared Variability Among YSOs in the Star Formation Region GGD12-15

We present an IR-monitoring survey with the Spitzer Space Telescope of the star-forming region GGD 12-15. More than 1000 objects were monitored, including about 350 objects within the central 5′, which is found to be especially dense in cluster members. The monitoring took place over 38 days and is part of the Young Stellar Object VARiability project. The region was also the subject of a contemporaneous 67 ks Chandra observation. The field includes 119 previously identified pre-main sequence star candidates. X-rays are detected from 164 objects, 90 of which are identified with cluster members. Overall, we find that about half the objects in the central 5′ are young stellar objects (YSOs) based on a combination of their spectral energy distribution, IR variability, and X-ray emission. Most of the stars with IR excess relative to a photosphere show large amplitude (>0.1 mag) mid-infrared (mid-IR) variability. There are 39 periodic sources, and all but one is found to be a cluster member. Almost half of the periodic sources do not show IR excesses. Overall, more than 85% of the Class I, flat spectrum, and Class II sources are found to vary. The amplitude of the variability is larger in more embedded YSOs. Most of the Class I/ II objects exhibit redder colors in a fainter state, which is compatible with time-variable extinction. A few become bluer when fainter, which can be explained with significant changes in the structure of the inner disk. A search for changes in the IR due to X-ray events is carried out, but the low number of flares prevented an analysis of the direct impact of X-ray flares on the IR light curves. However, we find that X-ray detected Class II sources have longer timescales for change in the MIR than a similar set of non-X-ray detected Class IIs.

YSOVAR: Mid-infrared Variability in NGC 1333

As part of the Young Stellar Object VARiability (YSOVAR) program, wemonitored NGC 1333 for ∼35 days at 3.6 and 4.5 μm using theSpitzer Space Telescope. We report here on the mid-infrared variabilityof the point sources in the ∼10‧ × ∼20‧ areacentered on 03:29:06, +31:19:30 (J2000). Out of 701 light curves ineither channel, we find 78 variables over the YSOVAR campaign. Abouthalf of the members are variable. The variable fraction for the mostembedded spectral energy distributions (SEDs) (Class I, flat) is higherthan that for less embedded SEDs (Class II), which is in turn higherthan the star-like SEDs (Class III). A few objects have amplitudes(10–90th percentile brightness) in [3.6] or [4.5] > 0.2 mag; amore typical amplitude is 0.1–0.15 mag. The largest color changeis >0.2 mag. There are 24 periodic objects, with 40% of them beingflat SED class. This may mean that the periodic signal is primarily fromthe disk, not the photosphere, in those cases. We find 9 variableslikely to be “dippers,” where texture in the disk occultsthe central star, and 11 likely to be “bursters,” whereaccretion instabilities create brightness bursts. There are 39 objectsthat have significant trends in [3.6]–[4.5] color over thecampaign, about evenly divided between redder-when-fainter (consistentwith extinction variations) and bluer-when-fainter. About a third of the17 Class 0 and/or jet-driving sources from the literature are variableover the YSOVAR campaign, and a larger fraction (∼half) are variablebetween the YSOVAR campaign and the cryogenic-era Spitzer observations(6–7 years), perhaps because it takes time for the envelope torespond to changes in the central source. The NGC 1333 brown dwarfs donot stand out from the stellar light curves in any way except there is amuch larger fraction of periodic objects (∼60% of variable browndwarfs are periodic, compared to ∼30% of the variables overall).

Comet 322P/SOHO 1: An asteroid with the smallest perihelion distance?

We observed comet 322P/SOHO 1 (P/1999 R1) from the ground and with the Spitzer Space Telescope when it was between 2.2 and 1.2 AU from the Sun. These are the first observations of any SOHO-discovered periodic comet by a non-solar observatory, and allow us to investigate its behavior under typical cometary circumstances. 322P appeared inactive in all images. Its lightcurve suggests a rotation period of 2.8+/-0.3 hr and has an amplitude greater than ~0.3 mag, implying a density of at least 1000 kg m$^{-3}$, considerably higher than that of any known comet. It has average colors of g'-r' = 0.52+/-0.04 and r'-i' = 0.04+/-0.09. We converted these to Johnson colors and found that the V-R color is consistent with average cometary colors, but R-I is somewhat bluer; these colors are most similar to V- and Q-type asteroids. Modeling of the optical and IR photometry suggests it has a diameter of 150-320 m and a geometric albedo of 0.09-0.42, with diameter and albedo inversely related. Our upper limits to any undetected coma are still consistent with a sublimation lifetime shorter than the typical dynamical lifetimes for Jupiter Family Comets. These results suggest that it may be of asteroidal origin and only active in the SOHO fields of view via processes different from the volatile-driven activity of traditional comets. If so, it has the smallest perihelion distance of any known asteroid.

Contribuição para a caracterização da emissão de nanopartículas em processos de soldadura e avaliação de riscos decorrentes do processo

Trabalho Final de Mestrado para obtenção do grau de Mestre em Engenharia Química e Biológica Ramo de processos químicos

Ruostumattoman teräksen käyttö ja käyttövaatimukset LNG:n varasto- ja kuljetusjärjestelmissä

On arvioitu, että koko maailmaa kattava energiantarve nousee 1,2 % vuosinopeudella. Asiaa ei kaunista se tosiasia, että valtaosa tänä päivänä tuotetusta energiasta (85 %) on lähtöisin fossiilisista polttoaineista. Päästöjen on arvioitu lisääntyvän 2005 – 2030 välisenä aikana noin 30 %, vaikka uusiutuvaa energiaa käytettäisiin ja prosessien hyötysuhteet paranisivat. Vuonna 2015 voimaan tuleva rikkidirektiivi on pakottanut asiantuntijat löytämään korvaavan energialähteen, joka vähentäisi päästöjen määrää, ja jota esiintyisi suurissa määrissä. Nesteytetty maakaasu, LNG, toteuttaa edellä mainitut ehdot. Tässä diplomityössä perehdytään LNG-teollisuuden arvoketjuun Suomessa sekä muualla maailmassa. Työssä pääpainona on selvittää ruostumattoman teräksen käyttömahdollisuuksia nykyisessä LNG-teollisuuden arvoketjussa sekä selvittää sen uusia sovelluskohteita LNG-alalla tulevaisuudessa. Diplomityössä on tehty laaja kirjallisuuskatsaus LNG:n arvoketjuun ja uuden EN 1.4420 ruostumattoman teräksen soveltuvuuteen kryogeenisissä lämpötiloissa. Työn aikana on myös tehty useita haastatteluja LNG-teollisuudessa toimivien henkilöiden kanssa. Menetelmäkokeita ja koehitsauksia on suoritettu näiden haastattelujen perusteella.

Galien, "de ingenio sanitatis; de crisi (91); de diebus criticis, (119); de accidente et morbo (139); de interioribus (162); de simplicibus medicinis (202)".

Saisi avec 6 autres mss en janvier 1797 dans la bibliothèque de l'abbaye bénédictine de San Benedetto in Polirone près de Mantoue, cf. cote du XVIIIe s. "MS n° 49" (f. de garde); Laffitte, Bulletin du Bibliophile, 1989/2, 300; Delisle, Cab. des mss., II, 414; — ex-libris du XVe s. "Iste liber est mei mag. Johannis Martini de Ferariis de Parma artium ac medicine doctoris" (292v)

Traité de Ponce sur l'art épistolaire (13), précédé d'un calendrier lunaire (1) et des Méditations de saint Bernard (7).

Quincye "Mss bibliothec. du marquis de Quincy venant de Mr Fevret de Fontette...", "Donné par le marquis de Quincy aux manuscrits du roy" (1); cf. B.n.F., Imprimés, D 5373, ex dono "Donné à la bibliotheque du roy 1770, le marquis de Quincye"

Chroniques françaises, Histoire d'Alexandre, etc.

Contient : Chronique de Normandie, depuis le duc Aubert jusqu'à Henri III, roi d'Angleterre ; Chronique française abrégée de GUILLAUME DE NANGIS, jusqu'à Philippe le Bel ; Chronologie des rois de France jusqu'à Charles VI ; suivie de notes latines : « De Anglia » (fol. 111) ; — « Le serment que le Chancelier de France doit faire, » etc. (fol. 112) ; Chronique des quatre premiers Valois (1327-1393), publiée par S. Luce (Paris, 1862, In 8°) ; Histoire d'Alexandre le Grand (Historia de præliis du Pseudo-Callisthènes), en français ; « Le livre des meurs du gouvernement des seigneurs, appelé les Secrés des secrés d'ARISTOTE » ; « Proposicion faicte de par l'Université de Paris devant nos seigneurs de France et tout le conseil assemblez pour la reformacion du royaume, l'an 1405, le samedi VIIe jour de novembre, par Me Jehan Jarson..., chancellier en l'eglise Nostre-Dame de Paris » ; Recueil de pièces concernant la Normandie. — « Carta Normannorum. » (19 mars 1314 [1315]) ; Vidimus du texte latin du traité de Troyes entre Henri V et Charles VI (21 mai 1420) ; « Pour remonstrer en brief que les habitans du duchié de Normandie et mesmement les bourgois, manans et habitans de la ville de Rouen, ne doivent estre trais en France, ne sont tenus de y sortir jur[i]diction ne y respondre... » — « Raciones précédentes fuerunt composite per mag. Johannem Doule, licenciatum In legibus, condam advocatum In parlamento et magistrum requestarum regis dominum de Neufville » ; Texte français du traité de Troyes (21 mai 1420) ; « Arrest ou declaraciun que ung prelat ou eglise peult acquérir en ses liefs », en faveur de l'abaye de St-Ouen de Rouen (1373 et 1375), etc ; « Confirmatio Cartæ Normannorum » (16 nov. 1423) ; « Decretum unionis orientalis Ecclesiæ cum occidentali, publicalum... In concilio Florentino... 1439 » ; « Copia bulle [Eugenii IV] conservatorie studii Cadomensis » (18 mai 1439) ; Au bas de ce feuillet on lit cette note, de première main : « Cronicas Normannie et Francie, ceterasque alias scripturassuperius scriptas varias materias continentes scribi fecit Robertus, abbas Sancti Michaelis In periculo maris, apud Rothomagum, In pluribus annis, et finaliter perfecit usque hic, anno Domini 1436 » ; Ex-libris : « Messire Joachin de Dinteville, chevalier de l'ordre du Roy et gentilhomme de sa chambre, m'a donné ce livre à Troyes, en febvrier 1578. » (Signature grattée)