Socio-Cultural Learning to Increase Student Engagement in Introduction to MIS

Introduction to Management Information Systems (MIS) is a challenging course to teach because of the broad expanse of rapidlychanging material, the centrality of the course to the business curriculum, students’ demand for interactive teaching rather than traditional lecture, and general student disinterest in or lack of familiarity with the subject. Further compounding these problems, faculty may not be adequately comfortable with or trained in active teaching modalities. To address these challenges, we used principles of socio-cultural learning to design a system of class activities to teach the dynamic concepts commonly found in the Introduction to MIS course. Faculty can adapt and customize this system to suit almost any teaching style without significant preparation. Capitalizing on students’ own experiences, we provide ad hoc activities that encourage students to work outside their comfort zone, to communicate and challenge material, to value their own expertise, and to gain confidence working independently. This paper specifically answers the call for more research explaining the “how” of teaching rather than the “what” and will prove useful and immediately actionable for novice and seasoned faculty alike

Teaching Tip: Socio-Cultural Learning to Increase Student Engagement in Introduction to MIS

Introduction to Management Information Systems (MIS) is a challenging course to teach because of the broad expanse of rapidly-changing material, the centrality of the course to the business curriculum, students’ demand for interactive teaching rather than traditional lecture, and general student disinterest in or lack of familiarity with the subject. Further compounding these problems, faculty may not be adequately comfortable with or trained in active teaching modalities. To address these challenges, we used principles of socio-cultural learning to design a system of class activities to teach the dynamic concepts commonly found in the Introduction to MIS course. Faculty can adapt and customize this system to suit almost any teaching style without significant preparation. Capitalizing on students’ own experiences, we provide ad hoc activities that encourage students to work outside their comfort zone, to communicate and challenge material, to value their own expertise, and to gain confidence working independently. This paper specifically answers the call for more research explaining the “how” of teaching rather than the “what” and will prove useful and immediately actionable for novice and seasoned faculty alike

A Time Purified Separated Antiproton Beam At The AGS

Physic

How unique is the Asymptotic Normalisation Coefficient (ANC) method?

The asymptotic normalisation coefficients (ANC) for the vertex $^{10}$B $\to$ $^9$Be + p is deduced from a set of different proton transfer reactions at different energies. This set should ensure the peripheral character of the reaction and availability of data for the elastic channels. The problems associated with the characteristics of the data and the analysis are discussed. For a subgroup of the set of available data, the uniqueness property of the extracted ANC is fulfilled. However, more measurements are needed before a definite conclusion can be drawn.Comment: 19 pages, 11 figures, to be published in Phys Rev

The Fading Optical Counterpart of GRB~970228, Six Months and One Year Later

We report on observations of the fading optical counterpart of the gamma-ray burst GRB 970228, made with the Hubble Space Telescope STIS CCD approximately six months after outburst and with the HST/NICMOS and Keck/NIRC approximately one year after outburst. The unresolved counterpart is detected by STIS at V=28.0 +/- 0.25, consistent with a continued power-law decline with exponent -1.14 +/- 0.05. The counterpart is located within, but near the edge of, a faint extended source with diameter ~0."8 and integrated magnitude V=25.8 +/- 0.25. A reanalysis of HST and NTT observations performed shortly after the burst shows no evidence of proper motion of the point source or fading of the extended emission. Only the extended source is visible in the NICMOS images with a magnitude of H=23.3 +/- 0.1. The Keck observations find K = 22.8 +/- 0.3. Several distinct and independent means of deriving the foreground extinction in the direction of GRB 970228 all agree with A_V = 0.75 +/- 0.2. After adjusting for Galactic extinction, we find that the size of the observed extended emission is consistent with that of galaxies of comparable magnitude found in the Hubble Deep Field (HDF) and other deep HST images. Only 2% of the sky is covered by galaxies of similar or greater surface brightness; therefore the extended source is almost certainly the host galaxy. Additionally, we find that the extinction-corrected V - H and V - K colors of the host are as blue as any galaxy of comparable or brighter magnitude in the HDF. Taken in concert with recent observations of GRB 970508, GRB 971214, and GRB 980703 our work suggests that all four GRBs with spectroscopic identification or deep multicolor broad-band imaging of the host lie in rapidly star-forming galaxies.Comment: 24 pages, Latex, 4 PostScript figures, to appear in the May 10 issue of The Astrophysical Journal (Note: displayed abstract is abridged

WFPC2 Observations of the Hubble Deep Field-South

The Hubble Deep Field-South observations targeted a high-galactic-latitude field near QSO J2233-606. We present WFPC2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared to a new catalog of the HDF-N that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman-break galaxies at z > 2 than the HDF-N. The star-formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z ~ 2.7, and a factor of 1.3 higher at z ~ 4.Comment: 93 pages, 25 figures; contains very long table

High-Mass X-ray Binaries and the Spiral Structure of the Host Galaxy

We investigate the manifestation of the spiral structure in the distribution of high-mass X-ray binaries (HMXBs) over the host galaxy. We construct the simple kinematic model. It shows that the HMXBs should be displaced relative to the spiral structure observed in such traditional star formation rate indicators as the Halpha and FIR emissions because of their finite lifetimes. Using Chandra observations of M51, we have studied the distribution of X-ray sources relative to the spiral arms of this galaxy observed in Halpha. Based on K-band data and background source number counts, we have separated the contributions from high-mass and low-mass X-ray binaries and active galactic nuclei. In agreement with model predictions, the distribution of HMXBs is wider than that of bright HII regions concentrated in the region of ongoing star formation. However, the statistical significance of this result is low, as is the significance of the concentration of the total population of X-ray sources to the spiral arms. We also predict the distribution of HMXBs in our Galaxy in Galactic longitude. The distribution depends on the mean HMXB age and can differ significantly from the distributions of such young objects as ultracompact HII regions.Comment: 18 pages, 6 figures; Astronomy Letters, Vol. 33, No. 5, 2007, pp. 299-30

PERFECT RECALL AND PRUNING IN GAMES WITH IMPERFECT INFORMATION 1

Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/72986/1/j.1467-8640.1996.tb00256.x.pd