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Volunteer involving organizations (VIOs) play a vital role in many societies. Yet, turnover among volunteers remains a persistent struggle and VIOs still do not have a good understanding of why volunteers leave. In response, we employed a mixed-methods approach to explore why volunteers consider leaving. By coding textual responses of Australian State Emergency Services and Scouting volunteers (n = 252 and 2235) on an annual engagement survey, we found seven overarching reasons to consider leaving these VIOs: Conflict, high demands and/or low resources, lack of fit, lack of inclusion, personal commitments and circumstances, poor communication and organizational practices, and poor leadership. When contrasted to the reasons that employees leave organizations for, the lack of inclusion and poor communication and organizational practices seem to be uniquely salient reasons that volunteers consider leaving for. Subsequently, guided by the Proximal Withdrawal States theory and using quantitative data from the Scouts sample, we investigated how reasons to consider turnover can predict turnover intentions and turnover behavior. First, volunteers in different withdrawal states cited different potential turnover reasons. For example, volunteers who ‘wanted to stay, but felt they had to leave’ cited personal commitments and circumstances more frequently than those in different withdrawal states. Second, we found that reasons to consider turnover explained little variance in turnover behavior one year later.

This multi-sample study (5 samples) revisited the content and factor structure of the Multidimensional Work Motivation Scale (MWMS) through exploratory structural equation modelling. Specifically, the operational representation of, and the relations between, the types of behavioural regulation were investigated as was their relation to theoretical outcomes. Results suggest the removal of three problematic items and show that work motivation, as measured by the MWMS, is best represented by a factor structure reflecting autonomous motivation, introjected and external regulation as well as amotivation. Furthermore, introjected regulation is more strongly represented by its avoidance subscale, whereas the two types of external regulation (material and social) are not distinguishable. Lastly, autonomous motivation is linked to optimal employee functioning (e.g., vigor/vitality, satisfaction, lower turnover intention). The two controlled types of regulation have differentiated relations with performance, but are both linked to poor employee health and turnover intention, with (avoidance) introjected regulation being a particularly important predictor. By revisiting the content of the MWMS and cross-validating its structure in five samples, this study provides an empirically adequate representation of the types of regulation and their outcomes. Suggestions for future research aimed at improving the content of the MWMS are also offered.

This multi-sample study (5 samples) revisited the content and factor structure of the Multidimensional Work Motivation Scale (MWMS) through exploratory structural equation modelling. Specifically, the operational representation of, and the relations between, the types of behavioural regulation were investigated as was their relation to theoretical outcomes. Results suggest the removal of three problematic items and show that work motivation, as measured by the MWMS, is best represented by a factor structure reflecting autonomous motivation, introjected and external regulation as well as amotivation. Furthermore, introjected regulation is more strongly represented by its avoidance subscale, whereas the two types of external regulation (material and social) are not distinguishable. Lastly, autonomous motivation is linked to optimal employee functioning (e.g., vigor/vitality, satisfaction, lower turnover intention). The two controlled types of regulation have differentiated relations with performance, but are both linked to poor employee health and turnover intention, with (avoidance) introjected regulation being a particularly important predictor. By revisiting the content of the MWMS and cross-validating its structure in five samples, this study provides an empirically adequate representation of the types of regulation and their outcomes. Suggestions for future research aimed at improving the content of the MWMS are also offered.

The importance and influence of feedback is well-established in the literature (Hattie, 2009). The purpose of feedback is to improve learning (Voerman, Meijer, Korthagen, & Simons, 2012) by reducing discrepancies (Hattie, 2007), closing gaps (Sadler, 2010), and improving one's knowledge, and skill acquisition (Moreno, 2004). However, there is disjuncture concerning the effectiveness of unilateral or one-way feedback. Unilateral feedback has been critiqued for its failure to productively engage, guide learning, and monitor performance (Price, Handley, & Millar, 2011; Sadler, 1989). Despite calls to focus feedback on student learning outcomes (Hattie, 2009; Voerman et al., 2012), a third of feedback interventions have reported a decrease in student performance (Kluger & DeNisi, 1996). Research informs that feedback that focuses on self instead of task inhibits learning (Kluger & DeNisi, 1996; Shute, 2008). On the other hand, feedback that focuses on self-regulation, task, and cognitive processing enhances learning (Hattie & Timperley, 2007; Shute, 2008). However, teachers are observed delivering one-way feedback, rather than facilitating learning (Blair & Ginty, 2013; Van den Berghe, Ros, & Beijaard, 2013), and appear ‘to close down opportunities for exploring student learning rather than opening them up’ (Torrance & Pryor, 1988, p. 621). That is, self-focussed unilateral feedbackthwarts the potential to promote learning (Burke, 2009)...

The importance and influence of feedback is well-established in the literature (Hattie, 2009). The purpose of feedback is to improve learning (Voerman, Meijer, Korthagen, & Simons, 2012) by reducing discrepancies (Hattie, 2007), closing gaps (Sadler, 2010), and improving one's knowledge, and skill acquisition (Moreno, 2004). However, there is disjuncture concerning the effectiveness of unilateral or one-way feedback. Unilateral feedback has been critiqued for its failure to productively engage, guide learning, and monitor performance (Price, Handley, & Millar, 2011; Sadler, 1989). Despite calls to focus feedback on student learning outcomes (Hattie, 2009; Voerman et al., 2012), a third of feedback interventions have reported a decrease in student performance (Kluger & DeNisi, 1996). Research informs that feedback that focuses on self instead of task inhibits learning (Kluger & DeNisi, 1996; Shute, 2008). On the other hand, feedback that focuses on self-regulation, task, and cognitive processing enhances learning (Hattie & Timperley, 2007; Shute, 2008). However, teachers are observed delivering one-way feedback, rather than facilitating learning (Blair & Ginty, 2013; Van den Berghe, Ros, & Beijaard, 2013), and appear ‘to close down opportunities for exploring student learning rather than opening them up’ (Torrance & Pryor, 1988, p. 621). That is, self-focussed unilateral feedbackthwarts the potential to promote learning (Burke, 2009)...

Teacher-student interactions are fundamental to learning outcomes. However, the facilitation of student-defined, in-class two-way feedback interaction is under-researched. The purpose of this paper is to share insights from Year 9 students (N = 32; age = 14–15 years), describing effective teacher’s two-way feedback interaction through Respectful Inquiry (RI; asking questions, question openness, and attentive listening). Small-focussed group interviews were conducted and transcripts were inductively analysed to represent the conceptualised effective student-described teacher behaviour and associated learning outcomes. Findings confirm that two-way feedback, as opposed to unilateral teacher feedback, is facilitative of more diverse and higher-order learning outcomes. According to the students, RI is constitutive in the two-way feedback interaction process; executed together, positive psychological needs support and metacognition are fostered. While this research was exploratory, the findings offer practical and novel insights on teachers’ two-way feedback interactions that can enhance students’ metacognition and suggests how specific feedback behaviours augment higher-order learning outcomes.

Teacher-student interactions are fundamental to learning outcomes. However, the facilitation of student-defined, in-class two-way feedback interaction is under-researched. The purpose of this paper is to share insights from Year 9 students (N = 32; age = 14–15 years), describing effective teacher’s two-way feedback interaction through Respectful Inquiry (RI; asking questions, question openness, and attentive listening). Small-focussed group interviews were conducted and transcripts were inductively analysed to represent the conceptualised effective student-described teacher behaviour and associated learning outcomes. Findings confirm that two-way feedback, as opposed to unilateral teacher feedback, is facilitative of more diverse and higher-order learning outcomes. According to the students, RI is constitutive in the two-way feedback interaction process; executed together, positive psychological needs support and metacognition are fostered. While this research was exploratory, the findings offer practical and novel insights on teachers’ two-way feedback interactions that can enhance students’ metacognition and suggests how specific feedback behaviours augment higher-order learning outcomes.

We observed NGC 1624-2, the O-type star with the largest known magnetic field Bp~20 kG), in X-rays with the ACIS-S camera onboard the Chandra X-ray Observatory. Our two observations were obtained at the minimum and maximum of the periodic Halpha emission cycle, corresponding to the rotational phases where the magnetic field is the closest to equator-on and pole-on, respectively. With these observations, we aim to characterise the star's magnetosphere via the X-ray emission produced by magnetically confined wind shocks. Our main findings are: (i) The observed spectrum of NGC 1624-2 is hard, similar to the magnetic O-type star Theta 1 Ori C, with only a few photons detected below 0.8 keV. The emergent X-ray flux is 30% lower at the Halpha minimum phase. (ii) Our modelling indicated that this seemingly hard spectrum is in fact a consequence of relatively soft intrinsic emission, similar to other magnetic Of?p stars, combined with a large amount of local absorption (~1-3 x 10^22 cm^-2). This combination is necessary to reproduce both the prominent Mg and Si spectral features, and the lack of flux at low energies. NGC 1624-2 is intrinsically luminous in X-rays (log LX emission ~ 33.4) but 70-95% of the X-ray emission produced by magnetically confined wind shocks is absorbed before it escapes the magnetosphere (log LX ISM corrected ~ 32.5). (iii) The high X-ray luminosity, its variation with stellar rotation, and its large attenuation are all consistent with a large dynamical magnetosphere with magnetically confined wind shocks., Comment: Accepted in MNRAS 13 pages, 10 figures, 4 tables

We observed NGC 1624-2, the O-type star with the largest known magnetic field Bp~20 kG), in X-rays with the ACIS-S camera onboard the Chandra X-ray Observatory. Our two observations were obtained at the minimum and maximum of the periodic Halpha emission cycle, corresponding to the rotational phases where the magnetic field is the closest to equator-on and pole-on, respectively. With these observations, we aim to characterise the star's magnetosphere via the X-ray emission produced by magnetically confined wind shocks. Our main findings are: (i) The observed spectrum of NGC 1624-2 is hard, similar to the magnetic O-type star Theta 1 Ori C, with only a few photons detected below 0.8 keV. The emergent X-ray flux is 30% lower at the Halpha minimum phase. (ii) Our modelling indicated that this seemingly hard spectrum is in fact a consequence of relatively soft intrinsic emission, similar to other magnetic Of?p stars, combined with a large amount of local absorption (~1-3 x 10^22 cm^-2). This combination is necessary to reproduce both the prominent Mg and Si spectral features, and the lack of flux at low energies. NGC 1624-2 is intrinsically luminous in X-rays (log LX emission ~ 33.4) but 70-95% of the X-ray emission produced by magnetically confined wind shocks is absorbed before it escapes the magnetosphere (log LX ISM corrected ~ 32.5). (iii) The high X-ray luminosity, its variation with stellar rotation, and its large attenuation are all consistent with a large dynamical magnetosphere with magnetically confined wind shocks., Comment: Accepted in MNRAS 13 pages, 10 figures, 4 tables

Building on results from the Magnetism in Massive Stars (MiMeS) project, this paper shows how a two-parameter classification of massive-star magnetospheres in terms of the magnetic wind confinement (which sets the Alfv\'en radius RA) and stellar rotation (which sets the Kepler co-rotation radius RK) provides a useful organisation of both observational signatures and theoretical predictions. We compile the first comprehensive study of inferred and observed values for relevant stellar and magnetic parameters of 64 confirmed magnetic OB stars with Teff > 16 kK. Using these parameters, we locate the stars in the magnetic confinement-rotation diagram, a log-log plot of RK vs. RA. This diagram can be subdivided into regimes of centrifugal magnetospheres (CM), with RA > RK, vs. dynamical magnetospheres (DM), with RK > RA. We show how key observational diagnostics, like the presence and characteristics of Halpha emission, depend on a star's position within the diagram, as well as other parameters, especially the expected wind mass-loss rates. In particular, we identify two distinct populations of magnetic stars with Halpha emission: namely, slowly rotating O-type stars with narrow emission consistent with a DM, and more rapidly rotating B-type stars with broader emission associated with a CM. For O-type stars, the high mass-loss rates are sufficient to accumulate enough material for line emission even within the relatively short free-fall timescale associated with a DM: this high mass-loss rate also leads to a rapid magnetic spindown of the stellar rotation. For the B-type stars, the longer confinement of a CM is required to accumulate sufficient emitting material from their relatively weak winds, which also lead to much longer spindown timescales. [abbreviated], Comment: Accepted for publication in MNRAS 30 pages, 10 figures, 6 tables

We report the detection of a strong, organized magnetic field in the secondary component of the massive O8III/I+O7.5V/III double-lined spectroscopic binary system HD 47129 (Plaskett's star), in the context of the Magnetism in Massive Stars (MiMeS) survey. Eight independent Stokes $V$ observations were acquired using the ESPaDOnS spectropolarimeter at the Canada-France-Hawaii Telescope and the Narval spectropolarimeter at the T\'elescope Bernard Lyot. Using Least-Squares Deconvolution we obtain definite detections of signal in Stokes $V$ in 3 observations. No significant signal is detected in the diagnostic null ($N$) spectra. The Zeeman signatures are broad and track the radial velocity of the secondary component; we therefore conclude that the rapidly-rotating secondary component is the magnetized star. Correcting the polarized spectra for the line and continuum of the (sharp-lined) primary, we measured the longitudinal magnetic field from each observation. The longitudinal field of the secondary is variable and exhibits extreme values of $-810\pm 150$ G and $+680\pm 190$ G, implying a minimum surface dipole polar strength of $2850\pm 500$ G. In contrast, we derive an upper limit ($3\sigma$) to the primary's surface magnetic field of 230 G. The combination of a strong magnetic field and rapid rotation leads us to conclude that the secondary hosts a centrifugal magnetosphere fed through a magnetically confined wind. We revisit the properties of the optical line profiles and X-ray emission - previously interpreted as a consequence of colliding stellar winds - in this context. We conclude that HD 47129 represents a heretofore unique stellar system - a close, massive binary with a rapidly rotating, magnetized component - that will be a rich target for further study., Comment: 10 pages, MNRAS, in press

This paper presents a first observational investigation of the faint Of?cp star NGC 1624-2, yielding important new constraints on its spectral and physical characteristics, rotation, magnetic field strength, X-ray emission and magnetospheric properties. Modeling the spectrum and spectral energy distribution, we conclude that NGC 1624-2 is a main sequence star of mass M {\simeq} 30 M{\odot}, and infer an effective temperature of 35 {\pm} 2 kK and log g = 4.0 {\pm} 0.2. Based on an extensive time series of optical spectral observations we report significant variability of a large number of spectral lines, and infer a unique period of 157.99 {\pm} 0.94 d which we interpret as the rotational period of the star. We report the detection of a very strong - 5.35 {\pm} 0.5 kG - longitudinal magnetic field , coupled with probable Zeeman splitting of Stokes I profiles of metal lines confirming a surface field modulus of 14 {\pm} 1 kG, consistent with a surface dipole of polar strength >~ 20 kG. This is the largest magnetic field ever detected in an O-type star, and the first report of Zeeman splitting of Stokes I profiles in such an object. We also report the detection of reversed Stokes V profiles associated with weak, high-excitation emission lines of O iii, which we propose may form in the close magnetosphere of the star. We analyze archival Chandra ACIS-I X-ray data, inferring a very hard spectrum with an X-ray efficiency log Lx/Lbol = -6.4, a factor of 4 larger than the canonical value for O-type stars and comparable to that of the young magnetic O-type star {\theta}1 Ori C and other Of?p stars. Finally, we examine the probable magnetospheric properties of the star, reporting in particular very strong magnetic confinement of the stellar wind, with {\eta}* {\simeq} 1.5 {\times} 10^4, and a very large Alfven radius, RAlf = 11.4 R*., Comment: 17 pages, MNRAS accepted and in press

Building on results from the Magnetism in Massive Stars (MiMeS) project, this paper shows how a two-parameter classification of massive-star magnetospheres in terms of the magnetic wind confinement (which sets the Alfv\'en radius RA) and stellar rotation (which sets the Kepler co-rotation radius RK) provides a useful organisation of both observational signatures and theoretical predictions. We compile the first comprehensive study of inferred and observed values for relevant stellar and magnetic parameters of 64 confirmed magnetic OB stars with Teff > 16 kK. Using these parameters, we locate the stars in the magnetic confinement-rotation diagram, a log-log plot of RK vs. RA. This diagram can be subdivided into regimes of centrifugal magnetospheres (CM), with RA > RK, vs. dynamical magnetospheres (DM), with RK > RA. We show how key observational diagnostics, like the presence and characteristics of Halpha emission, depend on a star's position within the diagram, as well as other parameters, especially the expected wind mass-loss rates. In particular, we identify two distinct populations of magnetic stars with Halpha emission: namely, slowly rotating O-type stars with narrow emission consistent with a DM, and more rapidly rotating B-type stars with broader emission associated with a CM. For O-type stars, the high mass-loss rates are sufficient to accumulate enough material for line emission even within the relatively short free-fall timescale associated with a DM: this high mass-loss rate also leads to a rapid magnetic spindown of the stellar rotation. For the B-type stars, the longer confinement of a CM is required to accumulate sufficient emitting material from their relatively weak winds, which also lead to much longer spindown timescales. [abbreviated], Comment: Accepted for publication in MNRAS 30 pages, 10 figures, 6 tables

We report the detection of a strong, organized magnetic field in the secondary component of the massive O8III/I+O7.5V/III double-lined spectroscopic binary system HD 47129 (Plaskett's star), in the context of the Magnetism in Massive Stars (MiMeS) survey. Eight independent Stokes $V$ observations were acquired using the ESPaDOnS spectropolarimeter at the Canada-France-Hawaii Telescope and the Narval spectropolarimeter at the T\'elescope Bernard Lyot. Using Least-Squares Deconvolution we obtain definite detections of signal in Stokes $V$ in 3 observations. No significant signal is detected in the diagnostic null ($N$) spectra. The Zeeman signatures are broad and track the radial velocity of the secondary component; we therefore conclude that the rapidly-rotating secondary component is the magnetized star. Correcting the polarized spectra for the line and continuum of the (sharp-lined) primary, we measured the longitudinal magnetic field from each observation. The longitudinal field of the secondary is variable and exhibits extreme values of $-810\pm 150$ G and $+680\pm 190$ G, implying a minimum surface dipole polar strength of $2850\pm 500$ G. In contrast, we derive an upper limit ($3\sigma$) to the primary's surface magnetic field of 230 G. The combination of a strong magnetic field and rapid rotation leads us to conclude that the secondary hosts a centrifugal magnetosphere fed through a magnetically confined wind. We revisit the properties of the optical line profiles and X-ray emission - previously interpreted as a consequence of colliding stellar winds - in this context. We conclude that HD 47129 represents a heretofore unique stellar system - a close, massive binary with a rapidly rotating, magnetized component - that will be a rich target for further study., Comment: 10 pages, MNRAS, in press

This paper presents a first observational investigation of the faint Of?cp star NGC 1624-2, yielding important new constraints on its spectral and physical characteristics, rotation, magnetic field strength, X-ray emission and magnetospheric properties. Modeling the spectrum and spectral energy distribution, we conclude that NGC 1624-2 is a main sequence star of mass M {\simeq} 30 M{\odot}, and infer an effective temperature of 35 {\pm} 2 kK and log g = 4.0 {\pm} 0.2. Based on an extensive time series of optical spectral observations we report significant variability of a large number of spectral lines, and infer a unique period of 157.99 {\pm} 0.94 d which we interpret as the rotational period of the star. We report the detection of a very strong - 5.35 {\pm} 0.5 kG - longitudinal magnetic field , coupled with probable Zeeman splitting of Stokes I profiles of metal lines confirming a surface field modulus of 14 {\pm} 1 kG, consistent with a surface dipole of polar strength >~ 20 kG. This is the largest magnetic field ever detected in an O-type star, and the first report of Zeeman splitting of Stokes I profiles in such an object. We also report the detection of reversed Stokes V profiles associated with weak, high-excitation emission lines of O iii, which we propose may form in the close magnetosphere of the star. We analyze archival Chandra ACIS-I X-ray data, inferring a very hard spectrum with an X-ray efficiency log Lx/Lbol = -6.4, a factor of 4 larger than the canonical value for O-type stars and comparable to that of the young magnetic O-type star {\theta}1 Ori C and other Of?p stars. Finally, we examine the probable magnetospheric properties of the star, reporting in particular very strong magnetic confinement of the stellar wind, with {\eta}* {\simeq} 1.5 {\times} 10^4, and a very large Alfven radius, RAlf = 11.4 R*., Comment: 17 pages, MNRAS accepted and in press

The Spitzer GLIMPSE and MIPSGAL surveys have revealed a wealth of details of the Galactic plane. We use them to study the energetics and dust properties of M16, one of the best known SFR. We present MIPSGAL observations of M16 at 24 and 70 $\mu$m and combine them with previous IR data. The MIR image shows a shell inside the molecular borders of the nebula. The morphologies at 24 and 70 $\mu$m are different, and its color ratio is unusually warm. The FIR image resembles the one at 8 $\mu$m that enhances the molecular cloud. We measure IR SEDs within the shell and the PDRs. We use the DUSTEM model to fit the SEDs and constrain dust temperature, dust size distribution, and ISRF intensity relative to that provided by the star cluster NGC6611. Within the PDRs, the dust temperature, the dust size distribution, and the ISRF intensity are in agreement with expectations. Within the shell, the dust is hotter and an ISRF larger than that provided by NGC6611 is required. We quantify two solutions. (1) The size distribution of the dust in the shell is not that of interstellar dust. (2) The dust emission arises from a hot plasma where UV and collisions with electrons contribute to the heating. We suggest two interpretations for the shell. (1) The shell matter is supplied by photo-evaporative flows arising from dense gas exposed to ionized radiation. The flows renew the shell matter as it is pushed by the stellar winds. Within this scenario, we conclude that massive SFR such as M16 have a major impact on the carbon dust size distribution. The grinding of the carbon dust could result from shattering in collisions within shocks driven by the interaction between the winds and the shell. (2) We consider a scenario where the shell is a SNR. We would be witnessing a specific time in the evolution of the SNR where the plasma pressure and temperature would be such that the SNR cools through dust emission., Comment: 15 pages, 18 figures, (almost) accepted for publication in A&A

The Spitzer GLIMPSE and MIPSGAL surveys have revealed a wealth of details of the Galactic plane. We use them to study the energetics and dust properties of M16, one of the best known SFR. We present MIPSGAL observations of M16 at 24 and 70 $\mu$m and combine them with previous IR data. The MIR image shows a shell inside the molecular borders of the nebula. The morphologies at 24 and 70 $\mu$m are different, and its color ratio is unusually warm. The FIR image resembles the one at 8 $\mu$m that enhances the molecular cloud. We measure IR SEDs within the shell and the PDRs. We use the DUSTEM model to fit the SEDs and constrain dust temperature, dust size distribution, and ISRF intensity relative to that provided by the star cluster NGC6611. Within the PDRs, the dust temperature, the dust size distribution, and the ISRF intensity are in agreement with expectations. Within the shell, the dust is hotter and an ISRF larger than that provided by NGC6611 is required. We quantify two solutions. (1) The size distribution of the dust in the shell is not that of interstellar dust. (2) The dust emission arises from a hot plasma where UV and collisions with electrons contribute to the heating. We suggest two interpretations for the shell. (1) The shell matter is supplied by photo-evaporative flows arising from dense gas exposed to ionized radiation. The flows renew the shell matter as it is pushed by the stellar winds. Within this scenario, we conclude that massive SFR such as M16 have a major impact on the carbon dust size distribution. The grinding of the carbon dust could result from shattering in collisions within shocks driven by the interaction between the winds and the shell. (2) We consider a scenario where the shell is a SNR. We would be witnessing a specific time in the evolution of the SNR where the plasma pressure and temperature would be such that the SNR cools through dust emission., Comment: 15 pages, 18 figures, (almost) accepted for publication in A&A

The Magnetism in Massive Stars (MiMeS) Project is a consensus collaboration among many of the foremost international researchers of the physics of hot, massive stars, with the basic aim of understanding the origin, evolution and impact of magnetic fields in these objects. At the time of writing, MiMeS Large Programs have acquired over 950 high-resolution polarised spectra of about 150 individual stars with spectral types from B5-O4, discovering new magnetic fields in a dozen hot, massive stars. The quality of this spectral and magnetic mat\'eriel is very high, and the Collaboration is keen to connect with colleagues capable of exploiting the data in new or unforeseen ways. In this paper we review the structure of the MiMeS observing programs and report the status of observations, data modeling and development of related theory., Comment: Proceedings of IAUS272: Active OB stars

The Magnetism in Massive Stars (MiMeS) Project is a consensus collaboration among many of the foremost international researchers of the physics of hot, massive stars, with the basic aim of understanding the origin, evolution and impact of magnetic fields in these objects. At the time of writing, MiMeS Large Programs have acquired over 950 high-resolution polarised spectra of about 150 individual stars with spectral types from B5-O4, discovering new magnetic fields in a dozen hot, massive stars. The quality of this spectral and magnetic mat\'eriel is very high, and the Collaboration is keen to connect with colleagues capable of exploiting the data in new or unforeseen ways. In this paper we review the structure of the MiMeS observing programs and report the status of observations, data modeling and development of related theory., Comment: Proceedings of IAUS272: Active OB stars