Learning Agility: In Search of Conceptual Clarity and Theoretical Grounding

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/92376/1/j.1754-9434.2012.01444.x.pd

RETROCAM: A Versatile Optical Imager for Synoptic Studies

We present RETROCAM, an auxiliary CCD camera that can be rapidly inserted into the optical beam of the MDM 2.4m telescope. The speed and ease of reconfiguring the telescope to use the imager and a straightforward user interface permit the camera to be used during the course of other observing programs. This in turn encourages RETROCAM's use for a variety of monitoring projects.Comment: 6 pages, 6 figures, Accepted by A

Learning Agility: Many Questions, a Few Answers, and a Path Forward

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/92383/1/j.1754-9434.2012.01465.x.pd

Personality Similarity in Negotiations: Testing the Dyadic Effects of Similarity in Interpersonal Traits and the Use of Emotional Displays on Negotiation Outcomes.

We build on the small but growing literature documenting personality influences on negotiation by examining how the joint disposition of both negotiators with respect to the interpersonal traits of agreeableness and extraversion influences important negotiation processes and outcomes. Building on similarity-attraction theory, we articulate and demonstrate how being similarly high or similarly low on agreeableness and extraversion leads dyad members to express more positive emotional displays during negotiation. Moreover, because of increased positive emotional displays, we show that dyads with such compositions also tend to reach agreements faster, perceive less relationship conflict, and have more positive impressions of their negotiation partner. Interestingly, these results hold regardless of whether negotiating dyads are similar in normatively positive (i.e., similarly agreeable and similarly extraverted) or normatively negative (i.e., similarly disagreeable and similarly introverted) ways. Overall, these findings demonstrate the importance of considering the dyad\u27s personality configuration when attempting to understand the affective experience as well as the downstream outcomes of a negotiation

Illuminating the ‘Face’ of Justice: A Meta‐Analytic Examination of Leadership and Organizational Justice

A significant body of research has described effective leader behaviours and has connected these behaviours to positive employee outcomes. However, this research has yet to be systematically integrated with organizational justice research to describe how leader behaviours inform justice perceptions. Therefore, we conduct a meta‐analysis (k = 166, N = 46,034) to investigate how three types of leader behaviours (task, relational, and change) inform four dimensions of organizational justice (procedural, distributive, interpersonal, and informational) referenced to the leader and to the organization. Further, we examine the joint impact of leader behaviours and justice perceptions on social exchange quality (i.e., leader–member exchange), task performance, and job satisfaction. Our results suggest that leader behaviours differentially inform leader‐ and organization‐focused justice perceptions, and the joint effect of leader behaviours and justice perceptions offer more nuanced explanations for outcomes.Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/147024/1/joms12402_am.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/147024/2/joms12402.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/147024/3/joms12402-sup-0001-TableS1.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/147024/4/joms12402-sup-0002-TableS2.pd

MACHO 96-LMC-2: Lensing of a Binary Source in the LMC and Constraints on the Lensing Object

We present photometry and analysis of the microlensing alert MACHO 96-LMC-2. The ~3% photometry provided by the Global Microlensing Alert Network follow--up effort reveals a periodic modulation in the lightcurve. We attribute this to binarity of the lensed source. Microlensing fits to a rotating binary source magnified by a single lens converge on two minima, separated by delta chi^2 ~ 1. The most significant fit X1 predicts a primary which contributes ~100% of the light, a dark secondary, and an orbital period (T) of 9.2 days. The second fit X2 yields a binary source with two stars of roughly equal mass and luminosity, and T = 21.2 days. The lensed object appears to lie on the upper LMC main sequence. We estimate the mass of the primary component of the binary system, M ~2 M_sun. For the preferred model X1, we explore the range of dark companions by assuming 0.1 M_sun and 1.4 M_sun objects in models X1a and X1b, respectively. We find lens velocities projected to the LMC in these models of v^hat_X1a = 18.3 +/- 3.1 km/s and v^hat_X1b = 188 +/- 32 k/ms. In both these cases, a likelihood analysis suggests an LMC lens is preferred over a Galactic halo lens, although only marginally so in model X1b. We also find v^hat_X2 = 39.6 +/- 6.1 k/ms, where the likelihood for the lens location is strongly dominated by the LMC disk. In all cases, the lens mass is consistent with that of an M-dwarf. The LMC self-lensing rate contributed by 96-LMC-2 is consistent with model self-lensing rates. (Abridged)Comment: 23 pages, including 3 tables and 6 figures; Accepted for publication in The Astrophysical Journa

The MACHO project: Microlensing Optical Depth towards the Galactic Bulge from Difference Image Analysis

We present the microlensing optical depth towards the Galactic bulge based on the detection of 99 events found in our Difference Image Analysis (DIA) survey. This analysis encompasses three years of data, covering ~ 17 million stars in ~ 4 deg^2, to a source star baseline magnitude limit of V = 23. The DIA technique improves the quality of photometry in crowded fields, and allows us to detect more microlensing events with faint source stars. We find this method increases the number of detection events by 85% compared with the standard analysis technique. DIA light curves of the events are presented and the microlensing fit parameters are given. The total microlensing optical depth is estimated to be tau_(total)= 2.43^(+0.39/-0.38) x 10^(-6) averaged over 8 fields centered at l=2.68 and b=-3.35. For the bulge component we find tau_(bulge)=3.23^(+0.52/-0.50) x 10^(-6) assuming a 25% stellar contribution from disk sources. These optical depths are in good agreement with the past determinations of the MACHO Alcock et al. (1997) and OGLE Udalski et al. (1994) groups, and are higher than predicted by contemporary Galactic models. We show that our observed event timescale distribution is consistent with the distribution expected from normal mass stars, if we adopt the stellar mass function of Scalo (1986) as our lens mass function. However, we note that as there is still disagreement about the exact form of the stellar mass function, there is uncertainty in this conclusion. Based on our event timescale distribution we find no evidence for the existence of a large population of brown dwarfs in the direction of the Galactic bulge.Comment: Updated references and corrected optical depth values. tau_tot= [2.91(+0.47/-0.45) -> 2.43^(+0.39/-0.38)] x 10^(-6) tau_bul = [3.88(+0.63/-0.60) -> 3.23^(+0.52/-0.50)] x 10^(-6

Microlensing Neutron Stars

We investigate the chances that neutron stars act as the lense in a gravitational microlensing event towards the galactic bulge or a spiral arm. The observation of neutron stars by means of gravitational microlensing would allow the estimation of neutron star masses independently of the property of being a pulsar in a binary system. We estimate the contribution of neutron stars to the optical depth and the lensing rate based on two different models of the pulsar distribution in the galaxy. Since only a small fraction of all neutron stars are pulsars, it is unlikely to find a pulsar that acts as a microlense by chance. A position comparison of known radio pulsars with observed microlensing candidates towards the galactic bulge and spiral arms shows no candidate pair, which is consistent with the theoretical expectation. To improve the probability of microlensing a pulsar, we suggest to search for gravitational microlensing events of known nearby high proper motion pulsars. The pulsar PSR J1932+1059 is a good candidate for an astrometric detection of gravitational lensing.Comment: 9 pages, 7 figures, includes note added in proof, A&A in pres

When Can Employees Have a Family Life? The Effects of Daily Workload and Affect on Work-Family Conflict and Social Behaviors at Home

This article presents a longitudinal examination of antecedents and outcomes of work-to-family conflict. A total of 106 employees participating in an experience-sampling study were asked to respond to daily surveys both at work and at home, and their spouses were interviewed daily via telephone for a period of 2 weeks. Intraindividual analyses revealed that employees ’ perceptions of workload predicted work-to-family conflict over time, even when controlling for the number of hours spent at work. Workload also influenced affect at work, which in turn influenced affect at home. Finally, perhaps the most interesting finding in this study was that employees ’ behaviors in the family domain (reported by spouses) were predicted by the employees ’ perceptions of work-to-family conflict and their positive affect at home

Improving the Prospects for Detecting Extrasolar Planets in Gravitational Microlensing in 2002

Gravitational microlensing events of high magnification have been shown to be promising targets for detecting extrasolar planets. However, only a few events of high magnification have been found using conventional survey techniques. Here we demonstrate that high magnification events can be readily found in microlensing surveys using a strategy that combines high frequency sampling of target fields with online difference imaging analysis. We present 10 microlensing events with peak magnifications greater than 40 that were detected in real-time towards the Galactic Bulge during 2001 by MOA. We show that Earth mass planets can be detected in future events such as these through intensive follow-up observations around the event peaks. We report this result with urgency as a similar number of such events are expected in 2002.Comment: 11 pages, 3 embedded ps figures including 2 colour, revised version accepted by MNRA