The Quaternary Geologic History of the Canadian Rocky Mountains

The Canadian Rocky Mountains figured prominently during the glacial history of western Canada. First as a western limit or boundary to the Laurentide Ice Sheet, second as an eastern margin of the Cordilleran Ice Sheet, and finally as a centre of local Montane ice. Throughout the Quaternary, complex interactions of glacier ice from these three ice sources markedly changed the physical form of the Rocky Mountains, Trench and Foothills areas. Investigations into the Quaternary history of this region have been ongoing since the beginning of the last century. Since about 1950, the number of studies performed in this area have increased significantly. This paper briefly reviews the historical accomplishments of Quaternary work in the region up to the period of about 1950. From this time to the present, individual study efforts are examined in detail according to the three geographic regions: 1) the northern Rocky Mountains (from the Liard Plateau south to the McGregor Plateau), 2) the central Rocky Mountains (from the McGregor Plateau south to the Porcupine Hills) and 3) the southern Rocky Mountains (from the Porcupine Hills south to the international border). In the northern region, geologic data suggest a maximum of two Rocky Mountain glaciations and only one Laurentide glaciation and no ice coalescence. In the central region, three of four Rocky Mountain events, and at least two Laurentide events are known. Only in the central region is there good evidence for ice coalescence, but the timing of this event is not clearly established. In the south, at least three Rocky Mountain episodes and a variable number of Laurentide episodes are recognized. There is no evidence for ice coalescence. A number of facts support the proposal that Cordilleran ice crossed the Continental Divide and joined with local Montane ice at several locations. However, this expansion of western ice occurred before the Late Wisconsinan in all areas but Jasper. In general, the chronological data presented suggest that the Late Wisconsinan glaciation in the Rocky Mountains was a short-lived event which started around or after 20 ka years ago and ended before 12 ka ago.Les montagnes Rocheuses ont constitué un cas particulier au cours de l'évolution glaciaire de l'ouest du Canada. Elles ont d'abord formé la limite occidentale de l'Inlandsis laurentidien, puis la limite orientale de l'Inlandsis de la Cordillère et finalement le centre d'une glaciation alpine locale. Tout au long du Quaternaire, les interactions complexes des glaces à partir de ces trois sources ont modifié de façon sensible l'aspect physique des Rocheuses, du sillon et du piémont. Les études sur l'évolution géologique de la région ont commencé au début du siècle dernier; beaucoup plus nombreuses depuis 1950, elles se sont également diversifiées. On résume d'abord les réalisations jusqu'aux années 50, puis on se penche plus particulièrement sur les travaux accomplis depuis lors dans : 1) la partie septentrionale (du plateau du Liard au plateau du McGregor, au sud); 2) la partie centrale (du plateau du McGregor aux collines Porcupine, au sud); et 3) la partie méridionale (des collines Porcupine à la frontière des É-U., au sud). Dans la partie septentrionale, les données géologiques montrent l'existence d'au plus deux glaciations issues des Rocheuses, une seule glaciation laurentidienne et aucune coalescence des glaces. Dans la partie centrale, on reconnaît l'existence de trois ou quatre glaciations issues des Rocheuses et au moins deux glaciations d'origine laurentidienne. On y observe des indices sur la coalescence des glaces, mais on ne sait pas exactement quand elle s'est produite. Dans le sud, on reconnaît l'existence d'au moins trois glaciations issues des Rocheuses et d'un nombre variable de glaciations d'origine laurentidienne. Il n'y aurait pas eu de coalescence. Un certain nombre de faits appuient l'hypothèse selon laquelle les glaces cordillérennes auraient traversé la ligne de partage des eaux en plusieurs points pour se joindre aux glaces alpines locales. Cependant, cette extension des glaces venant de l'ouest s'est produite avant le Wisconsinien supérieur dans tous les secteurs, sauf à Jasper. De façon générale, les données chronologiques indiquent que la glaciation du Wisconsinien supérieur a été de courte durée dans les Rocheuses (de 20 ka à 12 ka environ).Die kanadischen Rocky Mountains stellen einen Sonderfall in der glazialen Geschichte von Westkanada dar. Zuerst als eine westiiche Grenze oder Trennungslinie zur laurentidischen Eisdecke, dann als ein ôstlicher Rand der Kordilleren-Eisdecke, und schlieBlich als das Zentrum einer lokalen alpinen Vereisung. Während des ganzen Quaternärs haben komplexe Interaktionen von Gletschereis aus diesen drei Eisquellen die physikalische Form der Rocky Mountains, der Trench und Foothill-Gebiete signifikant veràndert. Untersuchungen der Quatemàr-Geschichte dieses Gebiets finden seit dem Beginn des letzten Jahrhunderts statt. Dieser Aufsatz gibt einen kurzen Ùberblick ùber die historischen Leistungen der Arbeit zum Quaternàr in dem Gebiet bis in die 50ger Jahre. Von diesem Zeitpunkt an bis heute werden individuelle Forschungs-bemùhungen im Detail untersucht und zwar zu drei geographischen Gebieten: nôrdlichen, zentralen und sûdlichen Rocky Mountains. Im nôrdlichen Gebiet weisen die geologischen Daten auf maximal zwei Rocky Mountain-Vereisungen und nur eine laurentidische Vereisung und auf keinen Eiszusammen-schluB. Im mittleren Gebiet sind drei von vier Rocky Mountain-Vereisungen und mindesten zwei laurentidische Vereisungen bekannt. Nur im mittleren Gebiet findet man einen klaren Nachweis fur EiszusammenschluB aber die Zeit fur diesen Vorgang kann nicht klar bes-timmt werden. Im Sùden kônnen mindestens drei Rocky Mountain-Vereisungen und eine variable Zahl von laurentidischen Vereisungen erkannt werden. Es gibt keinerlei Hinweis auf EiszusammenschluB. Eine Reihe von Fakten stùtzen die These, daB Eis von den Kordil-leren die Wasserscheidelinie ùberquerte und sich an einigen Plàtzen mit lokalem alpinem Eis vereinigte. Jedoch geschah dièse Ausdehnung westlichen Eises vor dem spâten Wisconsinum in alien Gebieten auBer in Jasper. Im allgemeinen zeigen die vorgelegten chronologischen Daten, daB die Spàt-Wisconsinum-Vereisung in den Rocky Mountains ein kurzlebiges Ereignis war, das vor etwa 20 ka Jahren oder danach begann und vor 12 ka Jahren endete

An Interpretation of Late Quaternary Glacial Flow Indicators in the Baie des Chaleurs Region, Northern New Brunswick

A sequence of late Quaternary geologic events in northern New Brunswick is determined from striation analysis derived from published data, open file reports, and field research conducted by the authors since 1985. These data are integrated with clast provenance and clast fabric trend analysis, as well as information from other studies in the surrounding area. South of the Baie des Chaleurs, a complicated Late Wisconsinan glacial history is preserved in the form of erosive features including nailhead striae, miniature crag-and-tails, and various scars, striations, and fractures. The rarity of sedimentary deposits and datable materials precludes simple stratigraphie interpretation. Based on over 1,000 striation sites, we conclude four major phases of glacial flow affected the area during the Late Wisconsinan: 1) an early flow to the southeast which reflects local Appalachian ice; 2) a second phase of glacial flow to the east indicating a Laurentide ice influence in western New Brunswick; 3) a third phase of glacial flow to the north-northeast, which may represent ice response to drawdown in the Baie des Chaleurs; and 4) a final multidirectional flow indicating localized ice response during the last stages of Late Wisconsinan glaciation. The absence of Canadian Shield erratics in northern New Brunswick is explained in terms of ice streaming along the St. Lawrence channel beneath a southward-flowing Laurentide Ice Sheet. Basal ice debris (including Shield erratics) was apparently truncated and removed by the obliquely flowing ice stream, leaving relatively clean ice in the Ice Sheet as it entered Gaspésie and ultimately New Brunswick.On a déterminé la séquence des événements géologiques du Quaternaire supérieur survenus dans le nord du Nouveau-Brunswick à partir de l'analyse des stries tirée de diverses sources. Au sud de la baie des Chaleurs, l'évolution glaciaire complexe du Wisconsinien supérieur peut être retracée à partir des formes d'érosion glaciaire dont les clouures, les crag-and-tails miniatures, les cicatrices de toutes sortes, les stries et les fractures. La rareté des sédiments et des matériaux pouvant être datés excluent toute interprétation fondée sur la stratigraphie. En s'appuyant sur plus de 1000 sites de stries, on croit que la région a connu quatre épisodes glaciaires pendant le Wisconsinien supérieur: 1 ) le premier mouvement, de faible importance, s'est fait vers le SE en provenance des Appalaches; 2) le deuxième écoulement glaciaire vers PE démontre la force des glaces laurentidiennes au nord du Nouveau-Brunswick; 3) le troisième mouvement glaciaire vers le NNE pourrait être une réaction à l'affaissement qui s'est produit dans la baie des Chaleurs; 4) le dernier mouvement multidirectionnel s'est fait à partir de calottes localisées pendant les derniers stades de la glaciation wisconsinienne. On explique l'absence des blocs erratiques dans le nord du Nouveau-Brunswick par un écoulement des glaces le long du chenal laurentien interrompant l'Inlandsis laurentidien s'écoulant vers le sud. Les débris glaciaires de fond (y compris les blocs erratiques du Bouclier) ont apparemment été tronqués et enlevés par un courant glaciaire oblique, épurant ainsi la glace qui pénétrait en Gaspésie, puis au Nouveau-Brunswick.Een Interpretatie van Laat-glaciale Ijsbewegingsindicaties in de Chaleur Bay Regio, Noord New Brunswick. De Kwartair geologische kartering van noord New Brunswick begon met de studies van Robert Chalmers aan het einde van de 19e eeuw. Sindsdien zijn verschillende pogingen gedaan om de glaciale geschiedenis van dit gebied te ontravelen en uiteindelijk zijn Chalmers ideeen herontdekt en aangepast aan moderne theorien en modellen van glaciale processen en isostasie. De afwezigheid van stratigrafische secties en de aanwezigheid van vêle glaciale erosieve en morphologische vormen heeft geleid tot de ontwikkeling van een "erosie-stratigrafie ". Deze informatie wordt gesteund door till lithologische en ges-teente orientatie studies. Het resultaat van dit gedetailleerde karterings project is de her-kenning van 4 verschillende ijs-bewegingen. Datering van deze gebeurtenissen is een probleem vanwege een gebrek aan dateer-bare materialen. Een eerste zuidoostelijke ijsbeweging is geregistreerd in het oostelijke deel van het gebied en in de Chaleur Coastal Plain. De tweede en sterkste gebeurtenis geeft een oostwaartse ijsbeweging te zien, die waarschijnlijk gedurende het gehele Wisconsinan (Weichselien) en mogelijk het gehele Pleistoceen van belang kan zijn geweest. Een derde ijsbeweging is in noord-oostelijke richt-ing in de Baie des Chaleurs. In een latere fase, lokale ijsbewegingen vonden plaats in verschillende richtingen vanaf de hooglanden en mogelijk vanuit Baie des Chaleurs. Er is een poging gedaan deze gebeurtenissen in een régionale context te plaatsen, waarin de interactie van de Laurentide Ice Sheet met het Appalachian Ice Complex en het concept van een Laurentian ijsstroomkanaal centraal staan

Birth and early evolution of a planetary nebula

The final expulsion of gas by a star as it forms a planetary nebula --- the ionized shell of gas often observed surrounding a young white dwarf --- is one of the most poorly understood stages of stellar evolution. Such nebulae form extremely rapidly (about 100 years for the ionization) and so the formation process is inherently difficult to observe. Particularly puzzling is how a spherical star can produce a highly asymmetric nebula with collimated outflows. Here we report optical observations of the Stingray Nebula which has become an ionized planetary nebula within the past few decades. We find that the collimated outflows are already evident, and we have identified the nebular structure that focuses the outflows. We have also found a companion star, reinforcing previous suspicions that binary companions play an important role in shaping planetary nebulae and changing the direction of successive outflows.Comment: 9 pages + 3 figures. To appear in Nature, 2 April 199

A survey for water maser emission towards planetary nebulae. New detection in IRAS 17347-3139

We report on a water maser survey towards a sample of 27 planetary nebulae (PNe) using the Robledo de Chavela and Medicina single-dish antennas, as well as the Very Large Array (VLA). Two detections have been obtained: the already known water maser emission in K 3-35, and a new cluster of masers in IRAS 17347-3139. This low rate of detections is compatible with the short life-time of water molecules in PNe (~100 yr). The water maser cluster at IRAS 17347-3139 are distributed on a ellipse of size ~ 0.2" x 0.1", spatially associated with compact 1.3 cm continuum emission (simultaneously observed with the VLA). From archive VLA continuum data at 4.9, 8.4, and 14.9 GHz, a spectral index alpha = 0.76 +- 0.03 is derived for this radio source, which is consistent with either a partially optically thick ionized region or with an ionized wind. However, the latter scenario can be ruled out on mass-loss considerations, thus indicating that this source is probably a young PN. The spatial distribution and the radial velocities of the water masers are suggestive of a rotating and expanding maser ring, tracing the innermost regions of a torus formed at the end of the AGB phase. Given that the 1.3 cm continuum emission peak is located near one of the tips of the major axis of the ellipse of masers, we speculate on a possible binary nature of IRAS 17347-3139, where the radio continuum emission could belong to one of the components and the water masers would be associated with a companion.Comment: Accepted by The Astrophysical Journal. 25 pages, 6 figure

Time-dependent ejection velocity model for the outflow of Hen 3--1475

We present 2D axisymmetric and 3D numerical simulations of the proto-planetary nebula Hen 3-1475, which is characterized by a remarkably highly collimated optical jet, formed by a string of shock-excited knots along the axis of the nebula. It has recently been suggested that the kinematical and morphological properties of the Hen 3-1475 jet could be the result of an ejection variability of the central source (Riera et al. 2003). The observations suggest a periodic variability of the ejection velocity superimposed on a smoothly increasing ejection velocity ramp. From our numerical simulations, we have obtained intensity maps (for different optical emission lines) and position-velocity diagrams, in order to make a direct comparison with the HST observations of this object. Our numerical study allows us to conclude that a model of a precessing jet with a time-dependent ejection velocity, which is propagating into an ISM previously perturbed by an AGB wind, can succesfully explain both the morphological and the kinematical characteristics of this proto-planetary nebula.Comment: Astronomy and Astrophysics (accepted) (8 figures

Photometry and low resolution spectroscopy of hot post-AGB candidates

We have obtained Johnson U, B, V and Cousins R, I photometry and low resolution spectra of a small sample of hot post-AGB candidates. Using the present data in combination with JHK data from 2MASS, infrared data from the MSX catalog and the IRAS fluxes, we have studied the spectral energy distribution (SED) of these stars. Using the DUSTY code we have estimated the dust temperatures, the distances to the stars, the mass-loss rates, angular radii of the inner boundary of the dust envelopes and dynamical ages from the tip of the AGB. These candidates have also been imaged through a narrow band H-alpha filter, to search for nebulosity around the central stars. Our H-alpha images revealed the bipolar morphology of the low excitation PN IRAS 17395-0841 with an angular extent of 2.8arcsec. The bipolar lobes of IRAS 17423-1755 in H-alpha were found to have an angular extent of 3.5arcsec (south-east lobe) and 2.2arcsec (north-west lobe). The dust envelope characteristics, low resolution spectrum and IRAS colors suggest that IRAS 18313-1738 is similar to the proto-planetary nebula (PPN) HD 51585. The SED of IRAS 17423-1755, IRAS 18313-1738 and IRAS 19127+1717 show a warm dust component (in addition to the cold dust) which may be due to recent and ongoing mass-loss.Comment: 20 pages, 6 figures, h-alpha figure compressed with XV, paper accepted for publication in Astronomy & Astrophysic

Differential Proper-Motion Study of the Circumstellar Dust Shell of the Enigmatic Object, HD 179821

HD179821 is an enigmatic evolved star that possesses characteristics of both a post-asymptotic giant branch star and a yellow hyper-giant, and there has been no evidence that unambiguously defines its nature. These two hypotheses are products of an indeterminate distance, presumed to be 1 kpc or 6 kpc. We have obtained the two-epoch Hubble Space Telescope WFPC2 data of its circumstellar shell, which shows multiple concentric arcs extending out to about 8 arcsec. We have performed differential proper-motion measurements on distinct structures within the circumstellar shell of this mysterious star in hopes of determining the distance to the object, and thereby distinguishing the nature of this enigmatic stellar source. Upon investigation, rather than azimuthal radially symmetric expansion, we discovered a bulk motion of the circumstellar shell of (2.41+-0.43, 2.97+-0.32) mas/yr. This corresponded to a translational ISM flow of (1.28+-0.95, 7.27+-0.75) mas/yr local to the star. This finding implies that the distance to HD 179821 should be rather small in order for its circumstellar shell to preserve its highly intact spherical structure in the presence of the distorting ISM flow, therefore favoring the proposition that HD 179821 is a post-AGB object.Comment: Accepted for publication in ApJ

From pre- to young Planetary Nebulae: radio continuum variability

Searching for variability, we have observed a sample of hot post-AGB stars and young Planetary Nebulae candidates with the Very Large Array at 4.8, 8.4, and 22.4 GHz. The sources had been previously detected in the radio continuum, which is a proof that the central stars have started ionising their circumstellar envelopes and an increase in radio flux with time can be expected as a result of the progression of the ionisation front. Such a behaviour has been found in IRAS 18062+2410, whose radio modelling has allowed us to determine that its ionised mass has increased from 10^{-4} to 3.3 10^{-4} M_sun in 8 years and its envelope has become optically thin at lower frequencies. Different temporal behaviours have been found for three other sources. IRAS 17423-1755 has shown a possibly periodic pattern and an inversion of its radio spectral index, as expected from a varying stellar wind. We estimate that the radio flux arises from a very compact region around the central star (10^{15} cm) with an electron density of 2 10^6 cm^{-3}. IRAS 22568+6141 and 17516-2525 have decreased their radio flux densities of about 10% per year over 4 years. While a linear increase of the flux density with time points out to the progression of the ionisation front in the envelope, decreases as well as quasi-periodic patterns may indicate the presence of unstable stellar winds/jets or thick dusty envelopes absorbing ionising photons.Comment: 9 pages, 5 figures, accepted for publication on MNRA