Emily Macdonald

We have discovered 21 new Type Ia supernovae (SNe Ia) with the Hubble Space Telescope (HST) and have used them to trace the history of cosmic expansion over the last 10 billion yr. These objects, which include 13 spectroscopically confirmed SNe Ia at z ≥ 1, were discovered during 14 epochs of reimaging of the GOODS fields North and South over 2 yr with the Advanced Camera for Surveys on HST. Together with a recalibration of our previous HST-discovered SNe Ia, the full sample of 23 SNe Ia at z ≥ 1 provides the highest redshift sample known. Combining these data with previous SN Ia data sets, we measured H(z) at discrete, uncorrelated epochs, reducing the uncertainty of H(z > 1) from 50% to under 20%, strengthening the evidence for a cosmic jerk—the transition from deceleration in the past to acceleration in the present. The unique leverage of the HST high-redshift SNe Ia provides the first meaningful constraint on the dark energy equation-of-state parameter at z ≥ 1. The result remains consistent with a cosmological constant [w(z) = −1] and rules out rapidly evolving dark energy (dw/dz ≫ 1). The defining property of dark energy, its negative pressure, appears to be present at z > 1, in the epoch preceding acceleration, with ~98% confidence in our primary fit. Moreover, the z > 1 sample-averaged spectral energy distribution is consistent with that of the typical SN Ia over the last 10 Gyr, indicating that any spectral evolution of the properties of SNe Ia with redshift is still below our detection threshold.

Aims.We study the relationship between the local environment of galaxies and their star formation rate (SFR) in the Great Observatories Origins Deep Survey, GOODS, at .

We present spectral energy distributions (SEDs), Spitzer colours, and infrared (IR) luminosities for 850-μm selected galaxies in the Great Observatories Origins Deep Survey Northern (GOODS-N) field. Using the deep Spitzer Legacy images and new data and reductions of the Very Large Array-Hubble Deep Field (VLA-HDF) radio data, we find statistically secure counterparts for 60 per cent (21/35) of our submillimetre (submm) sample, and identify tentative counterparts for another 12 objects. This is the largest sample of submm galaxies with statistically secure counterparts detected in the radio and with Spitzer. Half of the secure counterparts have spectroscopic redshifts, while the other half have photometric redshifts. We find that in most cases the 850-μm emission is dominated by a single 24-μm source, with a median flux density of 241 μJy, leading to a median 24-to-850-μm flux density ratio of 0.040. A composite rest-frame SED shows that the submm sources peak at longer wavelengths than those of local ultraluminous infrared galaxies (ULIRGs). Using a basic grey-body model, 850-μm selected galaxies appear to be cooler than local ULIRGs of the same luminosity. This demonstrates the strong selection effects, both locally and at high redshift, which may lead to an incomplete census of the ULIRG population. The SEDs of submm galaxies are also different from those of their high-redshift neighbours, the near-IR selected BzK galaxies, whose mid-IR-to-radio SEDs are more like those of local ULIRGs. Using 24-μm, 850-μm and 1.4-GHz observations, we fit templates that span the mid-IR through radio to derive the integrated IR luminosity (LIR) of the submm galaxies and find a median value of LIR(8–1000 μm) = 6.0 × 1012 L⊙. By themselves, 24-μm and radio fluxes are able to predict LIR reasonably well because they are relatively insensitive to temperature. However, the submm flux by itself consistently overpredicts LIR when using spectral templates which obey the local ULIRG temperature–luminosity relation. The shorter Spitzer wavelengths sample the stellar bump at the redshifts of the submm sources, and we find that the Spitzer photometry alone provides a model-independent estimate of the redshift, σ[Δz/(1 +z)]= 0.07. The median redshift for our secure submm counterparts is 2.0. Using X-ray and mid-IR data, only 5 per cent of our secure counterparts (1/21) show strong evidence for an active galactic nucleus dominating the LIR.

This article describes a class of robots—“arthrobots”—inspired, in part, by the musculoskeletal system of arthropods (spiders and insects, inter alia). Arthrobots combine mechanical compliance, lightweight and simple construction, and inexpensive yet scalable design. An exoskeleton, constructed from thin organic polymeric tubes, provides lightweight structural support. Pneumatic joints modeled after the hydrostatic joints of spiders provide actuation and inherent mechanical compliance to external forces. An inflatable elastomeric tube (a “balloon”) enables active extension of a limb; an opposing elastic tendon enables passive retraction. A variety of robots constructed from these structural elements demonstrate (i) crawling with one or two limbs, (ii) walking with four or six limbs (including an insect-like triangular gait), (iii) walking with eight limbs, or (iv) floating and rowing on the surface of water. Arthrobots are simple to fabricate and are able to operate safely in contact with humans.

We present measurements of the clustering properties of bright (L > L*) z~4 Lyman break galaxies (LBGs) selected from the Oxford-Dartmouth Thirty Degree Survey (ODT). We describe techniques used to select and evaluate our candidates and calculate the angular correlation function, which we find best fitted by a power law, ω(θ) =Awθ−β with Aw= 15.4 (with θ in arcsec), using a constrained slope of β= 0.8. Using a redshift distribution consistent with photometric models, we deproject this correlation function and find a comoving Mpc in a Ωm= 0.3 flat λ cosmology for iAB≤ 24.5. This corresponds to a linear bias value of (assuming σ8= 0.9). These data show a significantly larger r0 and b than previous studies at z~4. We interpret this as evidence that the brightest LBGs have a larger bias than fainter ones, indicating a strong luminosity dependence for the measured bias of an LBG sample. Comparing this against recent results in the literature at fainter (subL*) limiting magnitudes, and with simple models describing the relationship between LBGs and dark matter haloes, we discuss the implications on the implied environments and nature of LBGs. It seems that the brightest LBGs (in contrast with the majority subL* population) have clustering properties, and host dark matter halo masses, which are consistent with them being progenitors of the most massive galaxies today.

The Oxford–Dartmouth Thirty Degree Survey (ODTS) is a deep, wide, multiband imaging survey designed to cover a total of 30 deg2 in BV Ri′Z, with a subset of U- and K-band data, in four separate fields of 5–10 deg2 centred at 00:18:24 +34:52, 09:09:45 +40:50, 13:40:00 +02:30 and 16:39:30 +45:24. Observations have been made using the Wide Field Camera on the 2.5-m Isaac Newton Telescope (INT) in La Palma to average limiting depths (5σ Vega, aperture magnitudes) of U= 24.8, B= 25.6, V= 25.0, R= 24.6 and i′= 23.5, with observations taken in ideal conditions reaching the target depths of U= 25.3, B= 26.2, V= 25.7, R= 25.4 and i′= 24.6. The INT Z-band data were found to be severely effected by fringing and, consequently, are now being obtained at the MDM observatory in Arizona. A complementary K-band survey has also been carried out at MDM, reaching an average depth of K5σ≈ 18.5. At present, approximately 23 deg2 of the ODTS have been observed, with 3.5 deg2 of the K-band survey completed. This paper details the survey goals, field selection, observation strategy and data reduction procedure, focusing on the photometric calibration and catalogue construction. Preliminary photometric redshifts have been obtained for a subsample of the objects with R≤ 23. These results are presented alongside a brief description of the photometric redshift determination technique used. The median redshift of the survey is estimated to be z≈ 0.7 from a combination of the ODTS photometric redshifts and comparison with the redshift distributions of other surveys. Finally, galaxy number counts for the ODTS are presented which are found to be in excellent agreement with previous studies.

The high instantaneous luminosities expected following the upgrade of the Large Hadron Collider (LHC) to the High-Luminosity LHC (HL-LHC) pose major experimental challenges for the CMS experiment.A central component to allow efficient operation under these conditions is the reconstruction of charged particle trajectories and their inclusion in the hardwarebased trigger system.There are many challenges involved in achieving this: a large input data rate of about 20-40 Tb/s; processing a new batch of input data every 25 ns, each consisting of about 15,000 precise position measurements and rough transverse momentum measurements of particles ("stubs"); performing the pattern recognition on these stubs to find the trajectories; and producing the list of trajectory parameters within 4 µs.This paper describes a proposed solution to this problem, specifically, it presents a novel approach to pattern recognition and charged particle trajectory reconstruction using an all-FPGA solution.The results of an end-to-end demonstrator system, based on Xilinx Virtex-7 FPGAs, that meets timing and performance requirements are presented along with a further improved, optimized version of the algorithm together with its corresponding expected performance.

The relation between the lithium abundance, , and photospheric activity of solar-type Pleiads is investigated for the first time via acquisition and analysis of B and V-band data. Predictions of activity levels of target stars were made according to the ALi/ relation and then compared with new CCD photometric measurements. Six sources behaved according to the predictions while one star (HII 676), with low predicted activity, exhibited the largest variability of the study; another star (HII 3197), with high predicted activity, was surprisingly quiet. Two stars displayed non-periodic fadings, this being symptomatic of orbiting disk-like structures with irregular density distributions. Although the observation windows were not ideal for rotational period detection, some periodograms provided possible values; the light-curve obtained for HII 1532 is consistent with that previously recorded.

We present preliminary results from a programme to obtain multi‐object near‐infrared spectroscopy of galaxies at redshifts 0.7 < z < 1.5. We are using the instrument CIRPASS (the Cambridge Infra‐Red PAnoramic Survey Spectrograph), in multi‐object mode, to survey Hα in galaxies at z∼ 1. We aim to address the true star formation history of the Universe at this epoch: potentially the peak period of star formation activity. Hα is the same star formation measure used at low redshift, and hence we can trace star formation without the systematic uncertainties of using different calibrators in different redshift bins, or the extreme dust extinction in the rest‐ultraviolet (rest‐UV). CIRPASS has been successfully demonstrated in multi‐object mode on the Anglo‐Australian Telescope (AAT) and the William Herschel Telescope (WHT). Here we present preliminary results from one of our fields, the Hubble Deep Field North, observed with the WHT. With 150 fibres deployed over an unvignetted field of ∼15 arcmin, we have several detections of Hα from star‐forming galaxies at 0.8 < z < 1.0 and present spectra of the seven brightest of these. By pre‐selecting galaxies with redshifts such that Hα will appear between the OH sky lines, we can detect star formation rates of 5 h−270 M⊙ yr−1(5 σ in 3 hours, ΩM= 0.3, ΩΛ= 0.7). It appears that star formation rates inferred from Hα are, on average, a factor of more than two higher than those based on the UV continuum alone.

Assessing the environmental impact of the mineral extraction industry plays a critical role in understanding and mitigating the ecological consequences of extractive activities. This paper presents MineSegSAT, a model that presents a novel approach to predicting environmentally impacted areas of mineral extraction sites using the SegFormer deep learning segmentation architecture trained on Sentinel-2 data. The data was collected from non-overlapping regions over Western Canada in 2021 containing areas of land that have been environmentally impacted by mining activities that were identified from high-resolution satellite imagery in 2021. The SegFormer architecture, a state-of-the-art semantic segmentation framework, is employed to leverage its advanced spatial understanding capabilities for accurate land cover classification. We investigate the efficacy of loss functions including Dice, Tversky, and Lovasz loss respectively. The trained model was utilized for inference over the test region in the ensuing year to identify potential areas of expansion or contraction over these same periods. The Sentinel-2 data is made available on Amazon Web Services through a collaboration with Earth Daily Analytics which provides corrected and tiled analytics-ready data on the AWS platform. The model and ongoing API to access the data on AWS allow the creation of an automated tool to monitor the extent of disturbed areas surrounding known mining sites to ensure compliance with their environmental impact goals.

Chapter 31 A Census of Dust Absorption at the Galactic Centre Andy Adamson, Joint Astronomy Centre, Hilo, Hawaii 96720 U.S.A.Search for more papers by this authorRachel Mason, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UKSearch for more papers by this authorEmily Macdonald, University of Oxford, Department of Astrophysics, Keble Road, Oxford OX13RH, UKSearch for more papers by this authorGillian Wright, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UKSearch for more papers by this authorJean Chiar, NASA Ames Research Center, Mail stop 245–3, Moffett Field, CA 94035, USASearch for more papers by this authorYvonne Pendleton, NASA Ames Research Center, Mail stop 245–3, Moffett Field, CA 94035, USASearch for more papers by this authorTom Kerr, Joint Astronomy Centre, Hilo, Hawaii 96720 U.S.A.Search for more papers by this authorJanet Bowey, University College London, Dept. of Physics and Astronomy, Gower Street, London WC1E 6BT, UKSearch for more papers by this authorDoug Whittet, Rensselaer Polytechnic Institute, Department of Physics, Applied Physics and Astronomy, Troy, NY 12180Search for more papers by this authorMark Rawlings, Observatory, P.O. Box 14, University of Helsinki, FIN-00014 Helsinki, FinlandSearch for more papers by this author Andy Adamson, Joint Astronomy Centre, Hilo, Hawaii 96720 U.S.A.Search for more papers by this authorRachel Mason, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UKSearch for more papers by this authorEmily Macdonald, University of Oxford, Department of Astrophysics, Keble Road, Oxford OX13RH, UKSearch for more papers by this authorGillian Wright, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UKSearch for more papers by this authorJean Chiar, NASA Ames Research Center, Mail stop 245–3, Moffett Field, CA 94035, USASearch for more papers by this authorYvonne Pendleton, NASA Ames Research Center, Mail stop 245–3, Moffett Field, CA 94035, USASearch for more papers by this authorTom Kerr, Joint Astronomy Centre, Hilo, Hawaii 96720 U.S.A.Search for more papers by this authorJanet Bowey, University College London, Dept. of Physics and Astronomy, Gower Street, London WC1E 6BT, UKSearch for more papers by this authorDoug Whittet, Rensselaer Polytechnic Institute, Department of Physics, Applied Physics and Astronomy, Troy, NY 12180Search for more papers by this authorMark Rawlings, Observatory, P.O. Box 14, University of Helsinki, FIN-00014 Helsinki, FinlandSearch for more papers by this author Book Editor(s):Dr. A. Cotera, SETI Institute, Arizona State University, cotera@asu.eduSearch for more papers by this authorDr. S. Markoff, Max Planck Institute, Center for Space Research, smarkoff @ mpifr-bonn.mpg.deSearch for more papers by this authorT. R. Geballe, Gemini Observatory, tgeballe@gemini.eduSearch for more papers by this authorProf. Dr. H. Falcke, Max Planck Institute, Center for Space Research, falcke@astron.nlSearch for more papers by this author First published: 17 December 2003 https://doi.org/10.1002/9783527617982.ch31 AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onEmailFacebookTwitterLinked InRedditWechat Summary This chapter contains sections titled: Introduction Rationale Observations Modelling Summary Proceedings of the Galactic Center Workshop 2002: The Central 300 parsecs of the Milky Way RelatedInformation

OPEN ACCESSSeptember 28, 2012Transitioning From a Daily to a Block Didactic Format in a Pediatric Residency Program Walter Dehority, Amy Staples, Emily Macdonald, Jennifer Maito, Rebecca Rotello, Benjamin Hoffman Walter Dehority University of New Mexico Google Scholar More articles by this author , Amy Staples University of New Mexico Google Scholar More articles by this author , Emily Macdonald University of New Mexico Google Scholar More articles by this author , Jennifer Maito University of New Mexico Google Scholar More articles by this author , Rebecca Rotello University of New Mexico Google Scholar More articles by this author , Benjamin Hoffman Doernbecher Children's Hospital Google Scholar More articles by this author https://doi.org/10.15766/mep_2374-8265.9243 SectionsAbout ToolsDownload Citations ShareFacebookTwitterEmail AbstractAbstract Introduction: Prior to 2009, both faculty and housestaff at the University of New Mexico were dissatisfied with the structure of didactic instruction. Housestaff frequently missed daily noon-hour didactic sessions secondary to ongoing clinical duties. If residents were able to attend, both they and faculty presenters were frequently distracted by frequent pages. In response to this global dissatisfaction from housestaff and faculty about these daily noon didactic sessions, we sought to implement an alternative that would allow for truly protected resident time, regular attendance, and improved resident and faculty satisfaction. As a result, didactic instruction was transitioned to a block or “resident school” format, consisting of 4 hours of teaching held 1 day a week. A weekly block didactic format for residents has been utilized by some residency programs to combat many of the challenges that conspire to decrease the efficacy of didactic sessions. Methods: This resource describes the rationale and conceptual background for the transition into a block format, and provides instruction and guidance for programs interested in such a change. Example yearly and monthly templates, with the latter grouped by topic, are provided. A detailed discussion of the problems and limitations of the block format are also provided with potential solutions to common problems. Results: The introduction of a block didactic format in our Pediatric residency program was associated with significantly increased overall satisfaction when compared with a traditional daily didactic format by both housestaff and faculty. In addition, we witnessed a significant improvement in passage rates for the American Board of Pediatrics Certification examination among our graduates following implementation of the block didactic format, as well as improvements in in-training examination scores. We also demonstrated a 67% improvement in resident attendance with the transition to a block format by insuring that every resident who was eligible to attend did so each week. We demonstrated a significant improvement in resident satisfaction with the quality of faculty presentations after the format change, as well as a significant preference for the block format overall amongst both housestaff and faculty. Discussion: We believe our project is the first to assess the impact on faculty and housestaff of a transition from daily didactic sessions to a block didactic format, and the first to describe the implementation of a block didactic format in a program with intensive inpatient and outpatient service obligations. Such a format helps address several barriers to housestaff didactic education such as ongoing patient care and pager call, tasks identified in the literature to be the most likely to interfere with educational activities. This format also helps improve reported compliance with duty hour requirements, presumably because residents are able to focus on efficient clinical care without having to interrupt their workday to attend didactic sessions for all but one day of the week. Further, block didactics increased the punctuality of residents engaged in off-site clinical activities requiring extended travel time. Educational Objectives After implementing this resource, institutions will be able to: Improve housestaff attendance at weekly didactic sessions.Improve faculty and housestaff satisfaction with didactic offerings.Improve passage rates for the American Board of Pediatric Certification examination. Sign up for the latest publications from MedEdPORTAL Add your email below FILES INCLUDEDReferencesRelatedDetails FILES INCLUDED Included in this publication: Instructors Guide.docx Resource A - Resident School 12-Month Template.docx Resource B - Monthly Template for Resident School.docx Resource C - Example Template by Topic.docx Resource D - Faculty Opinions on the Transition to a Block Didactic Format.pptx Resource E - Housestaff Opinions on the Transition to a Block Didactic Format.pptx Resource F1 - Board passage rates.pptx Resource F2 - ITE scores.pptx Resource G1 - Resident pre-weekly didactic survey.pdf Resource G2 - Resident post-weekly didactic survey.pdf Resource G3 - Faculty pre-weekly didactic survey.pdf Resource G4 - Faculty post-weekly didactic survey.pdf To view all publication components, extract (i.e., unzip) them from the downloaded .zip file. Download editor’s noteThis publication may contain technology or a display format that is no longer in use. Copyright & Permissions© 2012 Dehority et al. This is an open-access article distributed under the terms of the Creative Commons Attribution license.KeywordsDidactic InstructionSchool Format Disclosures None to report. Funding/Support None to report. Loading ...

We report on a preliminary study concerning the origin of radio emission within radio galaxies at L(1.4GHz)>1E24 W/Hz in the GOODS-N field. In the local universe, Condon et al. (2002) and Yun et al. (2001) have shown that in galaxies with radio luminosities greater than 1E23 W/Hz the majority of the radio emission originates from a `monster' i.e., an AGN. Using the Chandra 2Msec X-ray image centered on the GOODS-N field and a reprocessed VLA HDF A-array data plus newly acquired VLA B-array data (rms=5.3microJy), we find that radio galaxies (with spectroscopic redshifts; all have z>1) with L(1.4GHz)>1E24 W/Hz typically have an X-ray detection rate of 72% (60% emit hard X-rays suggesting an AGN origin for the radio emission) in contrast to 25% for radio galaxies with L 1E24 W/Hz galaxies typically show compact rather than extended galaxy morphology which is generally found for the less luminous radio emitting galaxies but a few appear to be ongoing galaxy mergers. We also present SED fitting for these luminous radio galaxies including Spitzer IRAC & MIPS 24um photometry and 60% show distinct power-law SED indicative of an AGN. Initial results tell us that the X-ray emitting radio galaxy population are generally not submm sources but the few (~10%) that are SCUBA sources appear to be the small AGN population found by Pope et al. and others.

Abstract We present a flexible and scalable approach to address the challenges of charged particle track reconstruction in real-time event filters (Level-1 triggers) in collider physics experiments. The method described here is based on a full-mesh architecture for data distribution and relies on the Associative Memory approach to implement a pattern recognition algorithm that quickly identifies and organizes hits associated to trajectories of particles originating from particle collisions. We describe a successful implementation of a demonstration system composed of several innovative hardware and algorithmic elements. The implementation of a full-size system relies on the assumption that an Associative Memory device with the sufficient pattern density becomes available in the future, either through a dedicated ASIC or a modern FPGA. We demonstrate excellent performance in terms of track reconstruction efficiency, purity, momentum resolution, and processing time measured with data from a simulated LHC-like tracking detector.

Abstract Background In Norway, Legionnaires’ disease is reportable upon clinical suspicion to public health authorities and mandatorily notifiable through the Norwegian surveillance system for communicable diseases (MSIS) for both clinicians and laboratories. In the summer of 2017, several European countries reported high notification rates for Legionnaires’ disease, which was not observed in Norway. We evaluated MSIS to assess if it meets its objectives of detecting cases and trends in incidence of Legionnaires’ disease.Methods We retrieved MSIS data from 2008 to 2017 and calculated timeliness as days from sampling to notification, and internal completeness for key variables as the proportion of observations with a value. Where possible, we assessed internal validity on the presence of a plausible value. To estimate external completeness and validity we linked MSIS with hospital reimbursement claims in the Norwegian Patient Registry. To assess acceptability and representativeness, we surveyed doctors in 39 hospitals on their units’ diagnostic and notification procedures, and their use of MSIS.Results There were 438 notified cases. Internal completeness and internal validity were high for key variables (≥95%). The median delay from sampling to notification was 4 days. There were 73 patients in MSIS only, 70 in the Norwegian Patient Registry only, and 351 in both registers. The external completeness of MSIS was 83% (95% CI 80-86%). For external validity, the positive predictive value of MSIS was 83% (95% CI 79-86%). Forty-seven respondents from 28 hospitals described testing procedures. These were inconsistent: 29 (62%) reported no systematic application of criteria for requesting legionella testing. Eighteen (38%) reported testing all patients with suspected pneumonia and a travel history. Thirty-one (66%) found the notification criteria clear.Conclusions Our results suggest that the surveillance in MSIS can detect incidence changes for Legionnaires’ disease over time, by place and person, but likely does not detect every case diagnosed in Norway. We recommend wider investigation of diagnostic procedures in order to improve representativeness and awareness of MSIS notification criteria among clinicians in order to improve acceptability of the surveillance. We also recommend a more comprehensive assessment of whether patients only registered in the Norwegian Patient Registry were true Legionnaires’ disease cases.

Abstract Background In Norway, Legionnaire’s disease is reportable upon clinical suspicion to public health authorities and mandatorily notifiable through the Norwegian surveillance system for communicable diseases (MSIS) for both clinicians and laboratories. In the summer of 2017, several European countries reported high notification rates for Legionnaire’s disease, which was not observed in Norway. We evaluated MSIS to assess if it meets its objectives of detecting cases and trends in incidence of Legionnaire’s disease.Methods We retrieved MSIS data from 2008 to 2017 and calculated timeliness as days from sampling to notification, and internal completeness for key variables as the proportion of observations with a value. Where possible, we assessed internal validity on the presence of a plausible value. To estimate external completeness and validity we linked MSIS with hospital reimbursement claims in the Norwegian Patient Registry. To assess acceptability and representativeness, we surveyed doctors in 39 hospitals on their units’ diagnostic and notification procedures, and use of MSIS.Results There were 438 notified cases. Internal completeness and internal validity were high for key variables (≥95%). The median delay from sampling to notification was 4 days. There were 73 patients in MSIS only, 70 in the Norwegian Patient Registry only, and 351 in both registers. The external completeness of MSIS was 83% (95% CI 80-86%). For external validity, the positive predictive value of MSIS was 83% (95% CI 79-86%). Forty-seven respondents from 28 hospitals described testing procedures. These were inconsistent: 29 (62%) reported no systematic application of criteria for requesting legionella testing. Eighteen (38%) reported testing all patients with suspected pneumonia and a travel history. Thirty-one (66%) found the notification criteria clear.Conclusions Our results suggest that the surveillance in MSIS can detect changes in incidence of Legionnaire’s disease over time, by place and person, but likely does not detect every case diagnosed in Norway. We recommend wider investigation of diagnostic procedures in order to improve representativeness and awareness of MSIS notification criteria among clinicians in order to improve acceptability of the surveillance. We also recommend a more comprehensive assessment of whether patients only registered in the Norwegian Patient Registry were true Legionnaire’s disease cases.

We report on a preliminary study concerning the origin of radio emission within radio galaxies at L(1.4GHz)&gt;1E24 W/Hz in the GOODS-N field. In the local universe, Condon et al. (2002) and Yun et al. (2001) have shown that in galaxies with radio luminosities greater than 1E23 W/Hz the majority of the radio emission originates from a `monster' i.e., an AGN. Using the Chandra 2Msec X-ray image centered on the GOODS-N field and a reprocessed VLA HDF A-array data plus newly acquired VLA B-array data (rms=5.3microJy), we find that radio galaxies (with spectroscopic redshifts; all have z&gt;1) with L(1.4GHz)&gt;1E24 W/Hz typically have an X-ray detection rate of 72% (60% emit hard X-rays suggesting an AGN origin for the radio emission) in contrast to 25% for radio galaxies with L &lt; 1E23 W/Hz. The ACS images of these L(1.4 GHz) &gt; 1E24 W/Hz galaxies typically show compact rather than extended galaxy morphology which is generally found for the less luminous radio emitting galaxies but a few appear to be ongoing galaxy mergers. We also present SED fitting for these luminous radio galaxies including Spitzer IRAC &amp; MIPS 24um photometry and 60% show distinct power-law SED indicative of an AGN. Initial results tell us that the X-ray emitting radio galaxy population are generally not submm sources but the few (~10%) that are SCUBA sources appear to be the small AGN population found by Pope et al. and others.

We present the first successful demonstration of multi-object near-infrared spectroscopy on high redshift galaxies. Our objective is to address the true star formation history of the universe at z~1, a crucial epoch which some have suggested is the peak of star formation activity. By using H-alpha -the same robust star formation indicator used at low-z - redshifted into the J- and H-bands, we can trace star formation without the systematic uncertainties of different calibrators, or the extreme dust extinction in the rest-UV, which have plagued previous efforts. We are using the instrument CIRPASS (the Cambridge Infra-Red PAnoramic Survey Spectrograph), in multi-object mode, which has been successfully demonstrated on the Anglo-Australian Telescope (AAT) and the William Herschel Telescope (WHT). CIRPASS has 150 fibres deployable over \~40arcmin on the AAT and ~15arcmin on the WHT. Here we present preliminary results from one of our fields observed with the WHT: H-alpha detections of z~1 galaxies in the Hubble Deep Field North.

Astronomische NachrichtenVolume 324, Issue S1 p. 211-215 Chapter 3: Sagittarius A and its Environs A Census of Dust Absorption at the Galactic Centre Andy Adamson, Corresponding Author Andy Adamson a.adamson@jach.hawaii.edu Joint Astronomy Centre, Hilo, Hawaii 96720 U.S.A.Phone: +001 808 969 6511, Fax: +001 808 961 6516Search for more papers by this authorRachel Mason, Rachel Mason Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UKSearch for more papers by this authorEmily Macdonald, Emily Macdonald University of Oxford, Department of Astrophysics, Keble Road, Oxford OX13RH, UKSearch for more papers by this authorGillian Wright, Gillian Wright Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UKSearch for more papers by this authorJean Chiar, Jean Chiar NASA Ames Research Center, Mail stop 245-3, Moffett Field, CA 94035, USASearch for more papers by this authorYvonne Pendleton, Yvonne Pendleton NASA Ames Research Center, Mail stop 245-3, Moffett Field, CA 94035, USASearch for more papers by this authorTom Kerr, Tom Kerr Joint Astronomy Centre, Hilo, Hawaii 96720 U.S.A.Search for more papers by this authorJanet Bowey, Janet Bowey University College London, Dept. of Physics and Astronomy, Gower Street, London WC1E 6BT, UKSearch for more papers by this authorDoug Whittet, Doug Whittet Rensselaer Polytechnic Institute, Department of Physics, Applied Physics and Astronomy, Troy, NY 12180Search for more papers by this authorMark Rawlings, Mark Rawlings Observatory, P.O. Box 14, University of Helsinki, FIN-00014 Helsinki, FinlandSearch for more papers by this author Andy Adamson, Corresponding Author Andy Adamson a.adamson@jach.hawaii.edu Joint Astronomy Centre, Hilo, Hawaii 96720 U.S.A.Phone: +001 808 969 6511, Fax: +001 808 961 6516Search for more papers by this authorRachel Mason, Rachel Mason Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UKSearch for more papers by this authorEmily Macdonald, Emily Macdonald University of Oxford, Department of Astrophysics, Keble Road, Oxford OX13RH, UKSearch for more papers by this authorGillian Wright, Gillian Wright Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UKSearch for more papers by this authorJean Chiar, Jean Chiar NASA Ames Research Center, Mail stop 245-3, Moffett Field, CA 94035, USASearch for more papers by this authorYvonne Pendleton, Yvonne Pendleton NASA Ames Research Center, Mail stop 245-3, Moffett Field, CA 94035, USASearch for more papers by this authorTom Kerr, Tom Kerr Joint Astronomy Centre, Hilo, Hawaii 96720 U.S.A.Search for more papers by this authorJanet Bowey, Janet Bowey University College London, Dept. of Physics and Astronomy, Gower Street, London WC1E 6BT, UKSearch for more papers by this authorDoug Whittet, Doug Whittet Rensselaer Polytechnic Institute, Department of Physics, Applied Physics and Astronomy, Troy, NY 12180Search for more papers by this authorMark Rawlings, Mark Rawlings Observatory, P.O. Box 14, University of Helsinki, FIN-00014 Helsinki, FinlandSearch for more papers by this author First published: 20 October 2003 https://doi.org/10.1002/asna.200385097AboutPDF ToolsRequest permissionExport citationAdd to favoritesTrack citation ShareShare Give accessShare full text accessShare full-text accessPlease review our Terms and Conditions of Use and check box below to share full-text version of article.I have read and accept the Wiley Online Library Terms and Conditions of UseShareable LinkUse the link below to share a full-text version of this article with your friends and colleagues. Learn more.Copy URL Share a linkShare onFacebookTwitterLinked InRedditWechat Abstract The Galactic Centre offers a uniquely valuable line of sight for studies of the nature of dust in the ISM, but the long-held assumption that the line of sight samples only the diffuse ISM has been subverted by ground-based and ISO observations demonstrating the presence of absorption bands due to solid-phase volatile ices in the field. Spatial variability of the observed features suggests a patchy distribution of even the foreground diffuse-medium absorption. To map this clumpy distribution and to produce an inventory of the dust components, we are carrying out a narrow-band imaging survey over a field which extends from the Galactic Centre to beyond the circumnuclear ring, using both IRCAM3 and Michelle on UKIRT to cover the 3 μm water ice, 3.3 μm PAH, 3.4 μm hydrocarbon and 9.7 μm silicate absorption features. This paper presents the rationale for this programme and reports on progress with analysis of the survey data. Volume324, IssueS1Supplement: Proceedings of the Galactic Center Workshop 2002 – The central 300 parsecs of the Milky Way (Hardcover, ISBN 3-527-40466-X)September 2003Pages 211-215 RelatedInformation

The High-Luminosity LHC will open an unprecedented window on the weak-scale nature of the universe, providing high-precision measurements of the standard model as well as searches for new physics beyond the standard model.Such precision measurements and searches require information-rich datasets with a statistical power that matches the high luminosity provided by the Phase-2 upgrade of the LHC.Efficiently collecting those datasets will be a challenging task, given the harsh environment of 200 proton-proton interactions per LHC bunch crossing.For this purpose, CMS is designing an efficient data-processing hardware trigger (Level-1) that will include tracking information and high-granularity calorimeter information.The current conceptual system design is expected to take full advantage of FPGA and link technologies over the coming years, providing a high-performance, low-latency computing platform for large throughput and sophisticated data correlation across diverse sources.The envisaged L1 system will more closely replicate the full offline object reconstruction to perform a more sophisticated and optimized selection.Algorithms such as particle flow reconstruction can be implemented and complemented by standalone trigger object reconstruction.The expected performance and physics implications of such algorithms are studied using Monte Carlo samples with high pile-up, simulating the harsh conditions of the HL-LHC.The trigger object requirements are not only driven by the need to maintain physics selection thresholds to match those of the Phase-1, the selection of exotic signatures including displaced objects must be provided to help expand the physics reach of the experiment.The expected acceptance increase on selected benchmark signals obtained by the upgraded CMS Phase-2 Level-1 trigger will be summarized in this paper.