Identifying Contaminated K-band Globular Cluster RR Lyrae Photometry

Acquiring near-infrared K-band (2.2 um) photometry for RR Lyrae variables in globular clusters and nearby galaxies is advantageous since the resulting distances are less impacted by reddening and metallicity. However, K-band photometry for RR Lyrae variables in M5, Reticulum, M92, omega Cen, and M15 display clustercentric trends. HST ACS data imply that multiple stars in close proximity to RR Lyrae variables located near the cluster core, where the stellar density increases markedly, are generally unresolved in ground-based images. RR Lyrae variables near the cluster cores appear to suffer from photometric contamination, thereby yielding underestimated cluster distances and biased ages. The impact is particularly pernicious since the contamination propagates a systematic uncertainty into the distance scale, and hinders the quest for precision cosmology. The clustercentric trends are probably unassociated with variations in chemical composition since an empirical K-band period-magnitude relation inferred from Araucaria/VLT data for RR Lyrae variables in the Sculptor dSph exhibits a negligible metallicity dependence: (0.059+-0.095)[Fe/H], a finding that supports prior observational results. A future multi-epoch high-resolution near-infrared survey, analogous to the optical HST ACS Galactic Globular Cluster Survey, may be employed to establish K-band photometry for the contaminating stars discussed here.Comment: To appear in PAS

New ammonia masers towards NGC6334I

We report the detection of new ammonia masers in the non-metastable (8,6) and (11,9) transitions towards the massive star forming region NGC6334I. Observations were made with the ATCA interferometer and the emitting region appears unresolved in the 2.7" x 0.8" beam, with deconvolved sizes less than an arcsecond. We estimate peak brightness temperatures of 7.8 x 10^5 and 1.2 x 10^5 K for the (8,6) and (11,9) transitions, respectively. The masers appear coincident both spatially and in velocity with a previously detected ammonia (6,6) maser. We also suggest that emission in the (10,9), (9,9) and (7,6) transitions may also be masers, based on their narrow line widths and overlapping velocity ranges with the above masers, as observed with the single-dish Mopra radiotelescope

The molecular environment of massive star forming cores associated with Class II methanol maser emission

Methanol maser emission has proven to be an excellent signpost of regions undergoing massive star formation (MSF). To investigate their role as an evolutionary tracer, we have recently completed a large observing program with the ATCA to derive the dynamical and physical properties of molecular/ionised gas towards a sample of MSF regions traced by 6.7 GHz methanol maser emission. We find that the molecular gas in many of these regions breaks up into multiple sub-clumps which we separate into groups based on their association with/without methanol maser and cm continuum emission. The temperature and dynamic state of the molecular gas is markedly different between the groups. Based on these differences, we attempt to assess the evolutionary state of the cores in the groups and thus investigate the role of class II methanol masers as a tracer of MSF.Comment: 5 pages, 1 figure, IAU Symposium 242 Conference Proceeding

Hot high-mass accretion disk candidates

To better understand the physical properties of accretion disks in high-mass star formation, we present a study of a 12 high-mass accretion disk candidates observed at high spatial resolution with the Australia Telescope Compact Array (ATCA) in the NH3 (4,4) and (5,5) lines. Almost all sources were detected in NH3, directly associated with CH3OH Class II maser emission. From the remaining eleven sources, six show clear signatures of rotation and/or infall motions. These signatures vary from velocity gradients perpendicular to the outflows, to infall signatures in absorption against ultracompact HII regions, to more spherical infall signatures in emission. Although our spatial resolution is ~1000AU, we do not find clear Keplerian signatures in any of the sources. Furthermore, we also do not find flattened structures. In contrast to this, in several of the sources with rotational signatures, the spatial structure is approximately spherical with sizes exceeding 10^4 AU, showing considerable clumpy sub-structure at even smaller scales. This implies that on average typical Keplerian accretion disks -- if they exist as expected -- should be confined to regions usually smaller than 1000AU. It is likely that these disks are fed by the larger-scale rotating envelope structure we observe here. Furthermore, we do detect 1.25cm continuum emission in most fields of view.Comment: 21 pages, 32 figures, accepted for ApJS. A high-resolution version can be found at http://www.mpia.de/homes/beuther/papers.htm

Does Experience With Sagebrush in Utero and Early in Life Influence Use of Sagebrush by sheep?

Learning from mother begins early in the developmental process and can have lifelong effects when it comes to foraging behavior. Pregnancy is not just an incubation period but a starting point for animal well-being and disease later in life. A better understanding of the effects that early exposure to unpalatable feeds impinges on their use later in life may help create management plans that utilize grazing animals to their full potential as landscape manipulators. Thus, the objective of this research was to explore how experience in utero and early in life with sagebrush (Artemesia tridentata spp. tridentata) -a terpenoid-containing shrub- affected intake of and preference for sagebrush by sheep later in life. Eighty pregnant ewes (8 weeks of gestation) were divided into two groups, one group was exposed to sagebrush in their pens (25 to 30 Kg of freshly cut sagebrush was offered during 2-3 times a week), whereas the other group did not receive such exposure. Subsequently, lambs with their mothers were separated into four groups according to prior and subsequent exposure to sagebrush: 1) no exposure, 2) exposure in utero, 3) exposure in utero and for the first 2 mo. of life, and 4) exposure for the first 2 mo of life. At approximately 8 weeks of age, all lambs were weaned and four months later they were tested for their ability to ingest sagebrush. No differences regarding intake of sagebrush were detected among groups of lambs when they had choices between ad libitum amounts of alfalfa pellets and sagebrush (P \u3e 0.10). When the amounts of alfalfa pellets in the choice test were restricted to 50% of ad libitum intake, lambs in the group that only had in utero experience with sagebrush (Group 2) showed the lowest intakes of sagebrush (P \u3c 0.05). This suggests that in utero exposure to sagebrush decreased sagebrush preference and/or the ability of lambs to ingest this shrub. Sagebrush intake also increased across testing (P \u3c 0.05), suggesting that exposure to sagebrush during testing had a more pronounced effect on sagebrush intake than in utero or early life experiences with the shrub. In conclusion, prior experience with sagebrush under the conditions of the present study did not reveal an enhancement in sagebrush use later in life by sheep; on the contrary, in utero experiences with the shrub appeared to have reduced the ability of lambs to ingest sagebrush. Results from this study also suggest that exposing young lambs for several days to sagebrush while restricting the availability of high-quality forage is a viable option that may enhance utilization of sagebrush

Tracing the Conversion of Gas into Stars in Young Massive Cluster Progenitors

Whilst young massive clusters (YMCs; $M$ $\gtrsim$ 10$^{4}$ M$_{\odot}$, age $\lesssim$ 100 Myr) have been identified in significant numbers, their progenitor gas clouds have eluded detection. Recently, four extreme molecular clouds residing within 200 pc of the Galactic centre have been identified as having the properties thought necessary to form YMCs. Here we utilise far-IR continuum data from the Herschel Infrared Galactic Plane Survey (HiGAL) and millimetre spectral line data from the Millimetre Astronomy Legacy Team 90 GHz Survey (MALT90) to determine their global physical and kinematic structure. We derive their masses, dust temperatures and radii and use virial analysis to conclude that they are all likely gravitationally bound -- confirming that they are likely YMC progenitors. We then compare the density profiles of these clouds to those of the gas and stellar components of the Sagittarius B2 Main and North proto-clusters and the stellar distribution of the Arches YMC. We find that even in these clouds -- the most massive and dense quiescent clouds in the Galaxy -- the gas is not compact enough to form an Arches-like ($M$ = 2x10$^{4}$ M$_{\odot}$, R$_{eff}$ = 0.4 pc) stellar distribution. Further dynamical processes would be required to condense the resultant population, indicating that the mass becomes more centrally concentrated as the (proto)-cluster evolves. These results suggest that YMC formation may proceed hierarchically rather than through monolithic collapse.Comment: 12 pages, 8 figures, 1 table. Accepted by MNRA

Daylighting: appraisal at the early design stages

For a building design team concerned with the quality of the internal environment of buildings the percentage area of glazing on a building facade is one of the most useful criteria for judging the building envelope as a modifier of climate at early design stages since it is at the window that the various environmental parameters (heat, light and sound) remain only minimally modified. The percentage area of glazing can be used to relate the numerous and often conflicting functions of the window such as the provision of daylight, summer time teperatures, sound insulation, energy efficiency and view satisfaction