The Right to Know: Disclosure of Information for Collective Bargaining and Joint Consultation

The legal obligation on employers to provide information to employees has grown since the early 1970s. At that time, the emphasis was on disclosure for collective bargaining. In the 1980s and 1990s, the emphasis shifted more to disclosure for joint consultation. In the context of new legislation, the possibility of further interventions from Europe, and a greater commitment to openness in other areas of company and public life, disclosure of information for collective bargaining and joint consultation at work is again on the agenda. This article focuses on disclosure for both of these processes. Disclosure for collective bargaining is the most developed and potentially significant area of the law from an industrial relations perspective. Disclosure for joint consultation, however, has been the most dynamic area in recent years. Voluntary information provision by firms has also been a significant part of developing human resource management practice. The paper therefore provides a broad examination of the law on disclosure. The UK provisions are conceptualised as constituting an agenda-driven disclosure model; i.e. the trigger for their use lies within the bargaining agenda. By contrast, the provisions stemming from European initiatives are event-driven; i.e. they are triggered by specific employer initiated events that affect employment contracts in other ways irrespective of the representative context. In the final sections, we attempt a broader evaluation of the intent and impact of the legislation and assess the pros and cons of the different approaches.Disclosure of information, collective bargaining, joint consultation

The effect of surface temperature and Reynolds number on the leeward heat-transfer for a shuttle orbiter

The effect of windward surface temperature on the heat transfer to the leeward surface of the shuttle orbiter was investigated. Heat-transfer distributions, surface-pressure distributions, and schlieren photographs were obtained for an 0.01-scale model of the 37-0 shuttle orbiter at angles-of-attack of 30 deg and of 40 deg. Similar data were obtained for a fuselage-only configuration at angles-of-attack of 30 deg and of 90 deg. Data were obtained for various Mach numbers, Reynolds numbers, and surface temperatures

Forming Disk Galaxies in Lambda CDM Simulations

We used fully cosmological, high resolution N-body + SPH simulations to follow the formation of disk galaxies with rotational velocities between 135 and 270 km/sec in a Lambda CDM universe. The simulations include gas cooling, star formation, the effects of a uniform UV background and a physically motivated description of feedback from supernovae. The host dark matter halos have a spin and last major merger redshift typical of galaxy sized halos as measured in recent large scale N--Body simulations. The simulated galaxies form rotationally supported disks with realistic exponential scale lengths and fall on both the I-band and baryonic Tully Fisher relations. An extended stellar disk forms inside the Milky Way sized halo immediately after the last major merger. The combination of UV background and SN feedback drastically reduces the number of visible satellites orbiting inside a Milky Way sized halo, bringing it in fair agreement with observations. Our simulations predict that the average age of a primary galaxy's stellar population decreases with mass, because feedback delays star formation in less massive galaxies. Galaxies have stellar masses and current star formation rates as a function of total mass that are in good agreement with observational data. We discuss how both high mass and force resolution and a realistic description of star formation and feedback are important ingredients to match the observed properties of galaxies.Comment: Revised version after the referee's comments. Conclusions unchanged. 2 new plots. MNRAS in press. 20 plots. 21 page

An Orphan No Longer? Detection of the Southern Orphan Stream and a Candidate Progenitor

Using a shallow, two-color survey carried out with the Dark Energy Camera, we detect the southern, possibly trailing arm of the Orphan Stream. The stream is reliably detected to a decl. of −38°, bringing the total known length of the Orphan Stream to 108°. We find a slight offset or "S" shape in the stream at δ ≃ −14° that would be consistent with the transition from leading to trailing arms. This coincides with a moderate concentration of 137 ± 25 stars (to g = 21.6) that we consider a possible remnant of the Orphan progenitor. The position of this feature is in agreement with previous predictions

A Keck/DEIMOS spectroscopic survey of faint Galactic satellites: searching for the least massive dwarf galaxies

[abridged] We present the results of a spectroscopic survey of the recently discovered faint Milky Way satellites Boo, UMaI, UMaII and Wil1. Using the DEIMOS spectrograph on Keck, we have obtained samples that contain from 15 to 85 probable members of these satellites for which we derive radial velocities precise to a few km/s down to i~21-22. About half of these stars are observed with a high enough S/N to estimate their metallicity to within \pm0.2 dex. From this dataset, we show that UMaII is the only object that does not show a clear radial velocity peak. However, the measured systemic radial velocity (v_r=115\pm5 km/s) is in good agreement with recent simulations in which this object is the progenitor of the recently discovered Orphan Stream. The three other satellites show velocity dispersions that make them highly dark-matter dominated systems. In particular the Willman 1 object is not a globular cluster given its metallicity scatter over -2.0<[Fe/H]<-1.0 and is therefore almost certainly a dwarf galaxy or dwarf galaxy remnant. We measure a radial velocity dispersion of only 4.3_{-1.3}^{+2.3} km/s around a systemic velocity of -12.3\pm2.3 km/s which implies a mass-to-light ratio of ~700 and a total mass of ~5x10^5 Msun for this satellite, making it the least massive satellite galaxy known to date. Such a low mass could mean that the 10^7 Msun limit that had until now never been crossed for Milky Way and Andromeda satellite galaxies may only be an observational limit and that fainter, less massive systems exist within the Local Group. However, more modeling and an extended search for potential extra-tidal stars are required to rule out the possibility that these systems have not been significantly heated by tidal interaction.Comment: 24 pages, 11 figures, MNRAS accepte