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Applying a consideration set approach to panel data, we contribute to the literature on intra‐bloc voting by studying the vote for the Greens and the Social Democrats in the 2019 Swiss elections. Theoretically, because the two parties are ideologically and programmatically so similar, we argue that potential left‐wing voters have a hard time making a final choice based on issue positions, and rely instead on their evaluations of parties' issue competence. The empirical tests partly support our expectations. Maintaining or shifting the attribution of competence on the environment to the Greens during the election campaign prompts potential left‐wing voters to end up voting for the Greens; similar effects hold for the Social Democrats regarding social policy. Yet, this does not wipe out the impact of issue positions, which also help potential left‐wing voters decide between the Greens and the Social Democrats. These results have important theoretical and practical implications. Dieser Artikel leistet einen Beitrag zur Literatur über die Wahl von Parteien, die demselben politischen Lager angehören, indem er den sogenannten «consideration set»‐Ansatz auf die Stimmabgabe für die Grünen und die Sozialdemokraten bei den Schweizer Nationalratswahlen 2019 anwendet. Da diese zwei Parteien ideologisch und programmatisch sehr ähnlich sind, stellen wir die Hypothese auf, dass linke WählerInnen ihre endgültige Wahlentscheidung nur schwer auf der Grundlage ihrer Präferenzen für politische Themen treffen können und sich stattdessen auf ihre Wahrnehmung der Kompetenz der beiden Parteien in diesen Themen stützen. Diese Erwartungen werden teilweise empirisch bestätigt. Die Beibehaltung oder Verschiebung der Kompetenzzuweisung an die Grünen in Umweltfragen während der Wahlkampagne erhöht die Wahrscheinlichkeit, die Grünen zu wählen. Die Sozialisten profitieren von ähnlichen Effekten in Bezug auf die Sozialpolitik. Dies hebt jedoch nicht den Einfluss der Positionierung bezüglich Themen auf, welche ebenfalls dazu beiträgt, dass linke Wähler sich für die eine oder andere Partei entscheiden. Cet article contribue à la littérature sur le vote à l'intérieur d'un camp politique, en appliquant l'approche dite du « consideration set » au vote pour les Verts et les Socialistes aux élections fédérales de 2019. Dans la mesure où ces deux partis sont idéologiquement très similaires, nous faisons l'hypothèse que les électeur/trices de gauche ont du mal à faire leur choix final sur la base des préférences en matière d'enjeux politiques, et s'appuient à la place sur leur perception de la compétence des deux partis. Ces attentes sont partiellement confirmées empiriquement. Le maintien ou le déplacement de l'attribution de compétence en faveur des Verts sur l'environnement durant la campagne électorale augmente la probabilité de voter pour les Verts; les Socialistes bénéficient d'effets similaires en lien avec la politique sociale. Cependant, ceci ne supprime pas l'influence de la position sur les enjeux, qui aide aussi les votants de gauche à départager ces partis.

In light of the increased volatility in party preference and alleged importance of issue voting, the scarce knowledge about how short‐term stability and change in issue ownership perceptions influence stability and change of party choice is puzzling. This paper fills a gap by examining whether and to what extent the three pathways of electoral choice formation (activation, conversion and reinforcement) occur in line with the dynamics of issue competence evaluations. Our analysis of panel data from the 2015 Swiss election study shows that the stability and change in issue ownership perceptions is highly consequential. Citizens who change or maintain their competence attribution in favor of a party during the electoral campaign are more likely to activate, convert or reinforce their vote for that party. The results regarding the conditional effects of issue salience are more mixed, but not less interesting.

ABSTRACTGamesmanship is an act or verbal gesture used to psychologically unsettle opponents to gain an advantage in sport competition. Although verbal gamesmanship, colloquially known as trash talk, is most frequently used in the sports of ice hockey, American football, and basketball, it also has been found to occur in the game of golf. The purpose of this article is to help athletes, coaches, and sport psychologists to understand and develop strategies to cope with verbal gamesmanship in golf. To this end, verbal gamesmanship is described and the acronym PACE, theoretically grounded in a cognitive-behavioral approach, is presented as a tool that golfers can use to respond to verbal gamesmanship. PACE can help golfers to remind themselves to Pause, Assess, Concentrate, and Execute, all of which can be helpful when faced with verbal gamesmanship in golf settings.

•Athletic identity foreclosure is most pronounced during late adolescence.•It is responsive to changes in sport participation status.•It is related to a broad range of psychosocial factors.•It has been linked with substance use, career, burnout, and transition issues.

In the present work, we are interested in the three-dimensional description of the behaviour of a high strength material susceptible to adiabatic shear banding. The high strain rate constitutive model, based on irreversible thermodynamics, bas been formulated in order to be applied in the context of high velocity impact and penetration mechanics, and bas been implemented as `user material' in the finite element code LS-DYNA. Some preliminary numerical results are shown in the case of the loading of a plate hat specimen between Hopkinson pressure bars.

L'objectif industriel du travail dans lequel s'inscrit ce papier est la simulation numérique de la réponse de structures à l'impact. Or, pour un grand nombre de matériaux métalliques à haute résistance soumis à des sollicitations à grande vitesse, le cisaillement adiabatique constitue un processus endommageant conduisant souvent à la ruine par macrofissuration. Nous présentons ici un modèle continu qui, construit sur des bases thermodynamiques, rend compte du comportement thermo-élasto/viscoplastique du matériau sain et de l'anisotropie mécanique (dégradation directionnelle des modules élastiques et viscoplastiques induite par la présence des bandes de cisaillement adiabatique dans le matériau endommagé. Dans notre démarche de modélisation qui tend à refléter les constats expérimentaux, la population de bandes est représentée par une variable tensorielle d'endommagement au sein d'un matériau homogène équivalent. Le modèle est formulé dans le cadre des transformations finies élasto-plastiques avec prise en compte de l'anisotropie induite. Sa particularisation au cas des petites perturbations est illustrée pour certains processus homogènes.

We present the identification of a bright submillimeter (submm) source, SMM J163555.5+661300, detected in the lensing cluster Abell 2218, for which we have accurately determined the position using observations from the Submillimeter Array (SMA). The identified optical counterpart has a spectroscopic redshift of z = 4.044 +- 0.001 if we attribute the single emission line detected at l = 6140 A to Lya. This redshift identification is in good agreement with the optical/near-infrared photometric redshift as well as the submm flux ratio S 450/S 850[?] 1.6, the radio-submm flux ratio S 1.4/S 850 < 0.004, and the 24 mm to 850 mm flux ratio S 24/S 850 < 0.005. Correcting for the gravitational lensing amplification of [?]5.5, we find that the source has a far-infrared luminosity of 1.3 x 1012 L , which implies a star formation rate (SFR) of 230 M yr-1. This makes it the lowest-luminosity submillimeter galaxy (SMG) known at z>4 to date. Previous CO(4-3) emission line observations yielded a non-detection, for which we derived an upper limit of the CO line luminosity of $L_{\rm CO}^{^{\prime }} = 0.3\times 10^{10}$ K km s-1 pc-2, which is not inconsistent with the $L^{^{\prime }}_{\rm CO}$-L FIR relation for starburst galaxies. The best-fit model to the optical and near-infrared photometry give a stellar population with an age of 1.4 Gyr and a stellar mass of 1.6 x 1010 M . The optical morphology is compact and in the source plane the galaxy has an extent of [?]6 x 3 kpc with individual star-forming knots of <500 pc in size. J163556 is not resolved in the SMA data, and we place a strict upper limit on the size of the starburst region of 8 kpc x 3 kpc, which implies a lower limit on the SFR surface density of 12 M yr-1 kpc2. The redshift of J163556 extends the redshift distribution of faint, lensed SMGs, and we find no evidence that these have a different redshift distribution than bright SMGs.

We present results from a continuing interferometric survey of high-redshift submillimeter galaxies (SMGs) with the Submillimeter Array, including high-resolution (beam size [?]2 arcsec) imaging of eight additional AzTEC 1.1 mm selected sources in the COSMOS field, for which we obtain six reliable (peak signal-to-noise ratio (S/N) >5 or peak S/N >4 with multiwavelength counterparts within the beam) and two moderate significance (peak S/N >4) detections. When combined with previous detections, this yields an unbiased sample of millimeter-selected SMGs with complete interferometric follow up. With this sample in hand, we (1) empirically confirm the radio-submillimeter association, (2) examine the submillimeter morphology--including the nature of SMGs with multiple radio counterparts and constraints on the physical scale of the far infrared--of the sample, and (3) find additional evidence for a population of extremely luminous, radio-dim SMGs that peaks at higher redshift than previous, radio-selected samples. In particular, the presence of such a population of high-redshift sources has important consequences for models of galaxy formation--which struggle to account for such objects even under liberal assumptions--and dust production models given the limited time since the big bang.

We present a detailed comparison of the CO (3-2) emitting molecular gas between a local sample of luminous infrared galaxies (U/LIRGs) and a high-redshift sample that comprises submm selected galaxies (SMGs), quasars, and Lyman Break Galaxies (LBGs). The U/LIRG sample consists of our recent CO (3-2) survey using the Submillimeter Array while the CO (3-2) data for the high-redshift population are obtained from the literature. We find that the $L^{^{\prime }}_{\rm CO(3-2)}$ and L FIR relation is correlated over five orders of magnitude, which suggests that the molecular gas traced in CO (3-2) emission is a robust tracer of dusty star formation activity. The near unity slope of 0.93 +- 0.03 obtained from a fit to this relation suggests that the star formation efficiency is constant to within a factor of 2 across different types of galaxies residing in vastly different epochs. The CO (3-2) size measurements suggest that the molecular gas disks in local U/LIRGs (0.3-3.1 kpc) are much more compact than the SMGs (3-16 kpc), and that the size scales of SMGs are comparable to the nuclear separation (5-40 kpc) of the widely separated nuclei of U/LIRGs in our sample. We argue from these results that the SMGs studied here are predominantly intermediate stage mergers, and that the wider line widths arise from the violent merger of two massive gas-rich galaxies taking place deep in a massive halo potential.

We have used the Submillimeter Array (SMA) to make the first interferometric observations (beam size [?]1'' or [?]400 pc) of the 12CO J = 6 - 5 line and 435 mm (690 GHz) continuum emission toward the central region (half power field of view 17'') of the nearby ultra-luminous infrared galaxy (ULIRG) Arp 220. These observations resolve the eastern and western nuclei from each other, in both the molecular line and dust continuum emission. At 435 mm, the peak intensity of the western nucleus is stronger than the eastern nucleus, and the difference in peak intensities is less than at longer wavelengths. Fitting a simple model to the dust emission observed between 1.3 mm and 435 mm suggests that dust emissivity power law index in the western nucleus is near unity and steeper in the eastern nucleus, about 2, and that the dust emission is optically thick at the shorter wavelength. Comparison with single dish measurements indicate that the interferometer observations are missing [?]60% of the dust emission, most likely from a spatially extended component to which these observations are not sensitive. The 12CO J = 6 - 5 line observations clearly resolve kinematically the two nuclei. The distribution and kinematics of the 12CO J = 6 - 5 line appear to be very similar to lower J CO lies observed at similar resolution. Analysis of multiple 12CO line intensities indicates that the molecular gas in both nuclei have similar excitation conditions, although the western nucleus is warmer and denser. The excitation conditions are similar to those found in other extreme environments, including the nearby starburst galaxy M82, the active galactic nucleus (AGN) hosting ULIRG Mrk 231, and the high-z QSO BR 1202-0725. Simultaneous lower resolution observations of the 12CO, 13CO, and C18O J = 2 - 1 lines show that the 13CO and C18O lines have similar intensities, which suggests that both of these lines are optically thick, or possibly that extreme high mass star formation has produced in an overabundance of C18O.

We used the Submillimeter Array (SMA) to image 860 mm continuum and CO(3-2) line emission in the ultraluminous merging galaxy Arp 220, achieving a resolution of 0.23 '' (80 pc) for the continuum and 0.33 '' (120 pc) for the line. The CO emission peaks around the two merger nuclei with a velocity signature of gas rotation around each nucleus and is also detected in a kiloparsec-size disk encompassing the binary nucleus. The dust continuum, in contrast, is mostly from the two nuclei. The beam-averaged brightness temperature of both line and continuum emission exceeds 50 K at and around the nuclei, revealing the presence of warm molecular gas and dust. The dust emission morphologically agrees with the distribution of radio supernova features in the east nucleus, as expected when a starburst heats the nucleus. In the brighter west nucleus, however, the submillimeter dust emission is more compact than the supernova distribution. The 860 mm core, after deconvolution, has a size of 50-80 pc, consistent with recent 1.3 mm observations, and a peak brightness temperature of (0.9-1.6) x 102 K. Its bolometric luminosity is at least 2 x 1011 L and could be ~1012 L depending on source structure and 860 mm opacity, which we estimate to be of the order of t860 [?] 1 (i.e., NH2 [?] 1025 cm [?]2). The starbursting west nuclear disk must have in its center a dust enshrouded AGN or a very young starburst equivalent to hundreds of super star clusters. Further spatial mapping of bolometric luminosity through submillimeter imaging is a promising way to identify the heavily obscured heating sources in Arp 220 and other luminous infrared galaxies.

We present the results of a broadband simultaneous campaign on the nearby low-luminosity active galactic nucleus M81*. From 2005 February through August, we observed M81* five times using the Chandra X-Ray Observatory with the HETGS, complemented by ground-based observations with the Giant Meterwave Radio Telescope, the Very Large Array and Very Large Baseline Array, the Plateau de Bure Interferometer at IRAM, the Submillimeter Array, and Lick Observatory. We discuss how the resulting spectra vary over short and longer timescales compared to previous results, especially in the X-rays where this is the first ever longer term campaign at spatial resolution high enough to nearly isolate the nucleus (17 pc). We compare the spectrum to our Galactic center weakly active nucleus Sgr A*, which has undergone similar campaigns, as well as to weakly accreting X-ray binaries in the context of outflow-dominated models. In agreement with recent results suggesting that the physics of weakly accreting black holes scales predictably with mass, we find that the exact same model that successfully describes hard-state X-ray binaries applies to M81*, with very similar physical parameters.

We present ~2'' resolution CO (3-2), HCO+(4-3), and 880 mm continuum images of the luminous infrared galaxy NGC 6240 obtained at the Submillimeter Array. We find that the spatially resolved CO (3-2), HCO + (4-3), and the 880 mm emission peaks between the two nuclear components that are both known to harbor AGNs. Our large velocity gradient (LVG) analysis performed on each velocity channel suggests that the peak of the molecular gas emission traced in our observations is warm (T = 20-100 K), dense (nH2 = 105.0-105.4 cm-3), and moderately optically thin (t = 0.2-2) in the central 1 kpc. We also find large column densities of ~1023 cm-2. Such extreme conditions are observed over ~300 km s-1 centered around the CO-derived systemic velocity. The derived molecular gas mass from the CO (3-2) emission and a CO-to-H2 conversion factor commonly used for ULIRGs is (6.9 +- 1.7) x 109 M, and this is consistent with the mass derived from previous CO (2-1) observations. The gas is highly turbulent in the central kpc (DvFWZI ~ 1175 km s-1). Furthermore, possible inflow or outflow activity is suggested from the CO (3-2) velocity distribution. We tentatively state that 3.5 x 108 M of isolated CO (3-2) emission seen west of the northern disk may be associated with outflows from starburst superwinds, but the gas outflow scenario from one of the central AGN is not completely ruled out. Piecing all of the information together, the central region of NGC 6240 harbors 2 AGNs, ~1010 M of molecular gas mass, 5 x 107 M of dust mass, and has possible evidence of inflow and outflow activity.