The Evolution of Luminous Compact Blue Galaxies in COSMOS between z~0.0-1.0

Luminous Compact Blue Galaxies (LCBGs) are bright, compact star forming galaxies that are common in the distant universe, but rare locally. In this thesis we have conducted studies tracing changes in the LCBG population between z = 0.0--1.0 in the COSMOS survey region. We used the luminosity function to show LCBG\u27s contribution to the luminosity density is increasing between z = 0.0--1.0. From this we also find the number density of LCBGs is increasing by an order of magnitude from z = 0.0--1.0. Finally we show that 10% of galaxies brighter than MB = --18.5 are LCBGs at z ~ 0.1 but ~62% are LCBGs at z ~ 0.9 indicating LCBGs are a significant population of bright star forming galaxies at high redshift. In the second study we use the COSMOS HI Large Extragalactic Survey (CHILES) and CHILES Con Pol to trace star formation rate and HI in LCBGs to higher redshift. We determine the HI mass and distribution of two LCBGs in CHILES. We find the average star formation rate of LCBGs increases between z = 0.0--1.0 from 2 solar masses per year to 53 solar masses per year. Finally, we set upper limits on the evolution of the average HI mass in LCBGs between z = 0.0--0.45, which range from (2.3--5.6)x109 solar masses. In the last study we report on the first observations of HI in gravitationally lensed galaxies behind the galaxy cluster Abell 773. We find the upper limit for the average HI mass in the lensed galaxies at z = 0.398 to be 6.58 x 10 9 solar masses and the upper limit for the HI mass of the galaxy at z = 0.487 to be 1.5 x 1010 solar masses. We use an automated flagging routine to remove RFI which reduces the noise in the spectrum by ~25% when compared to spectrum in which we discarded integrations with RFI

An overt chemical protective garment reduces thermal strain compared with a covert garment in warm-wet but not hot-dry environments

© 2017 The Authors. Published by Frontiers Media. This is an open access article available under a Creative Commons licence. The published version can be accessed at the following link on the publisher’s website: https://doi.org/10.3389/fphys.2017.00913© 2017 Maley, Costello, Borg, Bach, Hunt and Stewart. Objectives: A commercial chemical, biological, radiological and nuclear (CBRN) protective covert garment has recently been developed with the aim of reducing thermal strain. A covert CBRN protective layer can be worn under other clothing, with equipment added for full chemical protection when needed. However, it is unknown whether the covert garment offers any alleviation to thermal strain during work compared with a traditional overt ensemble. Therefore, the aim of this study was to compare thermal strain and work tolerance times during work in an overt and covert ensemble offering the same level of CBRN protection. Methods: Eleven male participants wore an overt (OVERT) or covert (COVERT) CBRN ensemble and walked (4 km·h-1, 1% grade) for a maximum of 120 min in either a wet bulb globe temperature [WBGT] of 21, 30, or 37°C (Neutral, WarmWet and HotDry, respectively). The trials were ceased if the participants' gastrointestinal temperature reached 39°C, heart rate reached 90% of maximum, walking time reached 120 min or due to self-termination. Results: All participants completed 120 min of walking in Neutral. Work tolerance time was greater in OVERT compared with COVERT in WarmWet (P 0.05). Conclusion: Those dressed in OVERT experienced lower thermal strain and longer work tolerance times compared with COVERT in a warm-wet environment. However, COVERT may be an optimal choice in a hot-dry environment. These findings have practical implications for those making decisions on the choice of CBRN ensemble to be used during work.This project is financially supported by the Australian Government, managed by the National Security Science and Technology Centre within the Defence Science and Technology Organization, and the US Government through the Technical Support Working Group within the Combating Terrorism Technical Support Office.Published versio

Palaeomagnetism and magnetostiatigraphy of Triassic strata in the Sangre de Cristo Mountains and Tucumcari Basin, New Mexico, USA

We report palaeomagnetic data and a composite magnetic polarity sequence for Middle and Upper Triassic rocks assigned to the Anton Chico Member of the Moenkopi Formation and Chinle Group, respectively, exposed along the eastern flank of the Sangre de Cristo Mountains and in the Tucumcari Basin of eastern and northeastern New Mexico. Thermal demagnetization isolates a well-defined, dual polarity, characteristic magnetization, carried in most cases by haematite and interpreted as an early acquired chemical remanent magnetization (CRM). Characteristic magnetizations from 74 palaeomagnetic sites (one site = one bed) are used to define a magnetic polarity sequence, which we correlate with previously published Triassic data obtained from both marine and non-marine rocks. Preliminary correlation suggests that the resolution of magnetostratigraphic data derived from continental strata is not necessarily of lesser quality than that from marine rocks. On the basis of the magnetostratigraphic data, a profound unconformity is believed to separate lower-middle Norian and upper Norian-Rhaetian strata of the Chinle Group. Palaeomagnetic poles derived from selected sites in steeply dipping (> 85°) strata for the Middle Triassic (Anisian, ∼240 Ma: 50°N 121°E; N = 8), late Carman-early Norian (∼225 Ma: 53°N 104°E; N = 16), and late Norian-Rhaetian (∼208 Ma: 59°N 77°E; N = 8) are in relatively good agreement with previously published data for the Moenkopi Formation and Chinle Group and related strata in southwest North America. None the less, comparison with palaeomagnetic poles obtained from gently dipping or flat-lying Triassic strata from this study (Anisian, 46°N 112°E; N = 13; late Carnian, 54°N 87°E; N =12) and previously published Triassic poles in southwest North America suggest that a modest ‘apparent rotation’ not greater than about 5° affects declinations from steeply dipping rocks. The distribution of palaeomagnetic poles indicates ∼25° (angular distance) of apparent polar wander between about 240 and 208 Ma.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/73972/1/j.1365-246X.1996.tb05646.x.pd

Magnetostratigraphy and paleomagnetic poles from Late Triassic-earliest Jurassic strata of the Newark basin: Discussion and reply

The Discussion of Lucas and others underscores the potential usefulness of magnetostratigraphy for correlation between red beds of the broadly coeval Chinle Group of the western interior and the Newark Supergroup of eastern North America. Detailed magnetostratigraphic correlation between the Newark and the Chinle is very likely to change significantly, however, with the addition of new data from both of these units, and hence such an attempt as proposed in the Discussion may be premature

Assistive devices, hip precautions, environmental modifications and training to prevent dislocation and improve function after hip arthroplasty

This is the protocol for a review and there is no abstract. The objectives are as follows: The aim of this review is to assess the effects of provision of assistive devices, education on hip precautions, environmental modifications and training in ADL and EADL for people undergoing hip arthroplasty

Model-Independent Diagnostics of Highly Reddened Milky Way Star Clusters: Age Calibration

The next generation near- and mid-infrared Galactic surveys will yield a large number of new highly obscured star clusters. Detailed characterization of these new objects with spectroscopy is time-consuming. Diagnostic tools that will be able to characterize clusters based only on the available photometry will be needed to study large samples of the newly found objects. The brightness difference between the red clump and the main-sequence turn-off point have been used as a model-independent age calibrator for clusters with ages from a few 10$^8$ to 10$^{10}$ yr in the optical. Here we apply for the first time the method in the near-infrared. We calibrated this difference in $K$-band, which is likely to be available for obscured clusters, and we apply it to a number of test clusters with photometry comparable to the one that will be yielded by the current or near-future surveys. The new calibration yields reliable ages over the range of ages for which the red clump is present in clusters. The slope of the relation is smoother than that of the corresponding $V$-band relation, reducing the uncertainty in the age determinations with respect to the optical ones.Comment: 5 pages, 5 eps figure, accepted for publication in Astronomy and Astrophysic