The Lyman-alpha forest at redshifts 0.1 -- 1.6: good agreement between a large hydrodynamic simulation and HST spectra

We give a comprehensive statistical description of the Lyman-alpha absorption from the intergalactic medium in a hydrodynamic simulation at redshifts 0.1-1.6, the range of redshifts covered by HST spectra of QSOs. We use the ENZO code to make a 76 comoving Mpc cube simulation using 75 kpc cells, for a Hubble constant of 71 km/s/Mpc. The best prior work, by \citet{dave99},used an SPH simulation in a 15.6 Mpc box with an effective resolution of 245 kpc and slightly different cosmological parameters. At redshifts z=2 this simulation is different from data. \citet{tytler07b} found that the simulated spectra at z=2 have too little power on large scales, Lyman-alpha lines are too wide, there is a lack high column density lines, and there is a lack of pixels with low flux. Here we present statistics at z<1.6, including the flux distribution, the mean flux, the effective opacity, and the power and correlation of the flux. We also give statistics of the lyman alpha lines including the line width distribution, the column density distribution, the number of lines per unit equivalent width and redshift, and the correlation between the line width and column density. We find that the mean amount of absorption in the simulated spectra changes smoothly with redshift with DA(z)=0.01(1+z)^{2.25}. Both the trend and absolute values are close to measurements of HST spectra by \citet{kirkman07a}. The column density and line width distributions are also close to those measured from HST spectra by \citet{janknecht06a}, except for the mode of the line width distribution which is smaller in the HST spectra. Although some differences that we saw at z=2 are too subtle to be seen in existing HST spectra, overall, the simulation gives an good description of HST spectra at 0.1<z<1.6

The Effect of Large-Scale Power on Simulated Spectra of the Lya forest

We study the effects of box size on ENZO simulations of the intergalactic medium (IGM) at z = 2. We follow statistics of the cold dark matter (CDM) and the Lya absorption. We find that the larger boxes have fewer pixels with significant absorption (flux < 0.96) and more pixels in longer stretches with little or no absorption, and they have wider Lya lines. We trace these effect back to the additional power in larger boxes from longer wavelength modes. The IGM in our larger boxes is hotter, from increased pressure heating due to faster hydrodynamical infall. When we increase the photoheating in smaller boxes to compensate, their Lya statistics change to mimic those of a box of twice the size. Statistics converge towards their value in the largest (76.8 Mpc) box, except for the most common value of the CDM density which continues to rise. When we compare to errors with data, we find that our 76.8 Mpc box is larger than we need for the mean flux, barely large enough for the column density distribution and the power spectrum of the flux, and too small for the line widths. This box with 75 kpc cells has approximately the same mean flux as QSO spectra, but the Lya lines are too wide by 2.6 km/s, there are too few lines with log H I column densities > 10^17 cm^-2, and the power of the flux is too low by 20 - 50%, from small to large scales. Four times smaller cell size does not resolve these differences, nor do simple changes to the ultraviolet background that drives the H and He II ionization. It is hard to see how simulations using popular cosmological and astrophysical parameters can match Lyman-alpha forest data at z=2

Molecular functionalization of graphite surfaces : Basal Plane versus Step Edge electrochemical activity

The chemical functionalization of carbon surfaces has myriad applications, from tailored sensors to electrocatalysts. Here, the adsorption and electrochemistry of anthraquinone-2,6-disulfonate (AQDS) is studied on highly oriented pyrolytic graphite (HOPG) as a model sp2 surface. A major focus is to elucidate whether adsorbed electroactive AQDS can be used as a marker of step edges, which have generally been regarded as the main electroactive sites on graphite electrode surfaces. First, the macroscopic electrochemistry of AQDS is studied on a range of surfaces differing in step edge density by more than 2 orders of magnitude, complemented with ex situ tapping mode atomic force microscopy (AFM) data. These measurements show that step edges have little effect on the extent of adsorbed electroactive AQDS. Second, a new fast scan cyclic voltammetry protocol carried out with scanning electrochemical cell microscopy (SECCM) enables the evolution of AQDS adsorption to be followed locally on a rapid time scale. Subsequent AFM imaging of the areas probed by SECCM allows a direct correlation of the electroactive adsorption coverage and the actual step edge density of the entire working area. The amount of adsorbed electroactive AQDS and the electron transfer kinetics are independent of the step edge coverage. Last, SECCM reactive patterning is carried out with complementary AFM measurements to probe the diffusional electroactivity of AQDS. There is essentially uniform and high activity across the basal surface of HOPG. This work provides new methodology to monitor adsorption processes at surfaces and shows unambiguously that there is no correlation between the step edge density of graphite surfaces and the observed coverage of electroactive AQDS. The electroactivity is dominated by the basal surface, and studies that have used AQDS as a marker of steps need to be revised

Validity of the Actigraph GT9X Accelerometer Step-Count Function in Adults with Heart Failure with Preserved Ejection Fraction

Low physical activity is associated with heart failure with preserved ejection fraction (HFpEF). Step-counts, a measure of physical activity, can be measured via accelerometry. To date, few studies have examined validity of accelerometer-derived step-counts in the adults with HFpEF. PURPOSE To assess criterion validity of the Actigraph GT9X accelerometer step-count function in adults with HFpEF via ankle, waist, and wrist placement, compared with manually counted, directly observed steps. METHODS Six adults with HFpEF (age: 57.2 ± 9.4 y; African American: 50%; females: 100%) completed a cardiopulmonary exercise test (CPET) on a treadmill while wearing synchronized GT9X accelerometers on the ankle, waist, and wrist. Steps during CPET were measured by using the step-count function on the GT9X at 60 Hz sampling and data were downloaded into 1-second and 10-second epochs. Hand-tallied, directly observed steps (OS) was the criterion measure. Criterion validity was assessed via paired t tests to determine whether mean total steps (TS) from the three devices were significantly different from the mean TS from OS, and Pearson correlations were used to determine associations between device-measured TS and the total OS. Simple linear regression models were used to assess the effect of walking speed on absolute percentage error of the devices compared to OS. Agreement of the devices throughout the duration of the CPET was examined using Pearson correlations. Alpha was set at 0.05 for all statistical analyses. RESULTS Mean TS from waist-worn (t = -5.29, p = .001) and wrist-worn (t = -12.50, p \u3c .001) devices were significantly lower than mean TS from OS. Only TS from the ankle GT9X was significantly associated with TS from OS (r = 0.974, p = .001). GT9X-estimate steps from the ankle (r = 0.869, p \u3c .001), waist (r = 0.550, p \u3c.001), and wrist (r = 0.429, p \u3c.001) were all significantly associated with OS-measured steps. Absolute percentage error was significantly and negatively associated with treadmill speed for devices on the ankle (b = - 10.70, p \u3c .001), waist (b = -32.49, p \u3c .001) and wrist (b = -10.08, p \u3c .001). CONCLUSION Our results suggest that accelerometer-derived TS may be a more accurate measure of TS when the device is worn on the ankle rather than waist or wrist, and that measurement error is higher at lower walking speed.https://scholarscompass.vcu.edu/gradposters/1153/thumbnail.jp

Fluctuations of the intergalactic UV background towards two lines of sight

We present a reanalysis of the HeII Lyman alpha absorption towards the quasars HS1700+6416 and HE2347-4342 using new high S/N, optical observations. An alternative analysis method is applied, which fits the high quality, optical HI data directly to the HeII spectrum. The results are compared to those inferred from standard line profile analyses. This new method enables us to derive redshift scales characterizing the fluctuations of the column density ratio eta. We find eta changing smoothly with redshift on typical scales of Delta z ~ 0.01-0.03 corresponding to 8-24 h^-1 Mpc comoving. The real length scales of variations of the column density ratio might be even larger, since part of the fluctuations may be caused by noise in the HeII data and by effects due to the applied method. However, eta variations on small scales of a few Mpc with an amplitude of about +/- 1.5 dex cannot be ruled out completely. The data shows an apparent correlation between low eta regions and the presence of metal line absorbers, which corresponds to the more general correlation of low eta and strong HI absorption. Thermal line broadening is suggested as a probable explanation for this apparent correlation, since both fit methods would severely underestimate eta for absorbers with log N(HI) > 13 if the line width was dominated by thermal broadening. Indeed, lines located close to the cut-off of the b(N) distribution yield lower column density ratios compared to the whole sample, in particular if high density absorbers are considered. We argue that the apparent correlation of eta with the strength of the HI absorption is caused by insufficient consideration of thermal broadened lines by the standard analysis. As unbiased value of the column density ratio, we find eta ~80 in agreement with previous estimates.Comment: 15 pages, 11 figures, recommended for publication in A&

Hot Halos around High Redshift Protogalaxies: Observations of O VI and N V Absorption in Damped Lyman Alpha systems

(ABRIDGED) We present a study of the highly ionized gas (plasma) associated with damped Lyman-alpha (DLA) systems at z=2.1-3.1. We search for O VI absorption and corresponding Si IV, C IV, and N V in a Very Large Telescope/Ultraviolet-Visible Echelle Spectrograph (VLT/UVES) sample of 35 DLA systems with data covering O VI at S/N>10. We report twelve DLAs (nine intervening and three at <5000 km/s from the QSO redshift) with detections of O VI absorption. There are no clear O VI non-detections, so the incidence of O VI in DLAs is between 34% (12/35) and 100%. Analysis of the line widths together with photoionization modelling suggests that two phases of DLA plasma exist: a hot, collisionally ionized phase (seen in broad O VI components), and a warm, photoionized phase (seen just in narrow C IV and Si IV components). We find tentative evidence (98% confidence) for correlations between the DLA metallicity (measured in the neutral gas) and high-ion column density, and between the DLA metallicity and high-ion line width, as would be expected if supernova-driven galactic outflows rather than accretion produced the high ions. Using conservative ionization corrections, we find lower limits to the total hydrogen column densities in the hot (O VI-bearing) and warm (C IV-bearing) phases in the range log N(Hot H II) >19.5 to >21.1, and log N(Warm H II) >19.4 to >20.9. On average, the hot and warm phases thus contain >40% and >20% of the baryonic mass of the neutral phase in DLAs, respectively. If the temperature in the O VI phase is ~10^6 K and so f(O VI)=O VI/O<<0.2 the plasma can make a significant contribution to the metal budget at high redshift.Comment: 18 pages, 7 figures (3 in color), accepted to A&

The Deuterium to Hydrogen Abundance Ratio Towards a Fourth QSO: HS0105+1619

We report the measurement of the primordial D/H abundance ratio towards QSO \object. The column density of the hydrogen in the $z \simeq 2.536$ Lyman limit system is high, \lnhi $= 19.422 \pm 0.009$ \cmm, allowing for the deuterium to be seen in 5 Lyman series transitions. The measured value of the D/H ratio towards QSO \object is found to be D/H$= 2.54 \pm 0.23 \times 10^{-5}$. The metallicity of the system showing D/H is found to be $\simeq 0.01$ solar, indicating that the measured D/H is the primordial D/H within the measurement errors. The gas which shows D/H is neutral, unlike previous D/H systems which were more highly ionized. Thus, the determination of the D/H ratio becomes more secure since we are measuring it in different astrophysical environments, but the error is larger because we now see more dispersion between measurements. Combined with prior measurements of D/H, the best D/H ratio is now D/H$= 3.0 \pm 0.4 \times 10^{-5}$, which is 10% lower than the previous value. The new values for the baryon to photon ratio, and baryonic matter density derived from D/H are $\eta = 5.6 \pm 0.5 \times 10^{-10}$ and \ob $=0.0205 \pm 0.0018$ respectively.Comment: Minor text and reference changes. To appear in the May 10, 2001 issue of the Astrophysical Journa

DEMONSTRATING ADAPTABILITY: ROLE MODELLING MULTIDISCIPLINARY LEARNING IN THE LAB, ONLINE AND AT HOME

In this paper we analyse changes required in the role of laboratory demonstrators to support students across a mid-semester move to online learning in response to COVID-19. ‘Multidisciplinary Laboratories’ is a large (~450 students) first-year, multi-campus course at the University of Newcastle that is organised around two multifaceted investigations: ‘Water – would you drink it?’, and ‘Energy – can it be sustainable?’. The course introduces students each week to diverse disciplinary perspectives, i.e. Environmental Science and Management, Biology, Chemistry, Psychology, Human Geography, Earth Sciences, and Physics. The teaching cohort in each laboratory session (~45 students) comprises a discipline-specific academic lead that changes weekly, and two demonstrators who remain with the class for the whole semester. As laboratories moved online, demonstrators supported students’ learning through synchronous live classes, experiments at home, virtual experiments and asynchronous materials including video tutorials. Importantly, demonstrators have role-modelled for students adaptability under conditions of uncertainty. Analysis of evaluative data including Blackboard engagement records, student surveys and demonstrators’ observations suggests effectively supporting students’ learning required nuanced and important changes in demonstrators’ roles including technical aspects, and techniques for engaging students and facilitating classes

Wavelength Accuracy of the Keck HIRES Spectrograph and Measuring Changes in the Fine Structure Constant

We report on an attempt to accurately wavelength calibrate four nights of data taken with the Keck HIRES spectrograph on QSO PHL957, for the purpose of determining whether the fine structure constant was different in the past. Using new software and techniques, we measured the redshifts of various Ni II, Fe II, Si II, etc. lines in a damped Ly-alpha system at z=2.309. Roughly half the data was taken through the Keck iodine cell which contains thousands of well calibrated iodine lines. Using these iodine exposures to calibrate the normal Th-Ar Keck data pipeline output we found absolute wavelength offsets of 500 m/s to 1000 m/s with drifts of more than 500 m/s over a single night, and drifts of nearly 2000 m/s over several nights. These offsets correspond to an absolute redshift of uncertainty of about Delta z=10^{-5} (Delta lambda= 0.02 Ang), with daily drifts of around Delta z=5x10^{-6} (Delta lambda =0.01 Ang), and multiday drifts of nearly Delta z=2x10^{-5} (0.04 Ang). The causes of the wavelength offsets are not known, but since claimed shifts in the fine structure constant would result in velocity shifts of less than 100 m/s, this level of systematic uncertainty makes may make it difficult to use Keck HIRES data to constrain the change in the fine structure constant. Using our calibrated data, we applied both our own fitting software and standard fitting software to measure (Delta alpha)/alpha, but discovered that we could obtain results ranging from significant detection of either sign, to strong null limits, depending upon which sets of lines and which fitting method was used. We thus speculate that the discrepant results on (Delta alpha)/alpha reported in the literature may be due to random fluctuations coming from under-estimated systematic errors in wavelength calibration and fitting procedure.Comment: 19 pages, 10 figures, to appear in ApJ, Dec 2009 Many corrections and changes made, some new figure

Spectral shape of the UV ionizing background and HeII absorption at redshifts 1.8 < z < 2.9

The shape of the UV ionizing background is reconstructed from optically thin metal absorption-line systems identified in spectra of HE2347-4342, Q1157+3143, and HS1700+6416 in the redshift interval 1.8 < z < 2.9. The systems are analyzed by means of the Monte Carlo Inversion method completed with the spectral shape recovering procedure. The UVB spectral shape fluctuates at 2.4 < z < 2.9 mostly due to radiative transfer processes in the clumpy IGM. At z < 1.8, the IGM becomes almost transparent both in the HI and HeII Lyman continua and the variability of the spectral shape comes from diversity of spectral indices describing the QSO/AGN intrinsic radiation. At z > 2.4, the recovered spectral shapes show intensity depression between 3 and 4 Ryd due to HeII Ly-alpha absorption in the IGM clouds (line blanketing) and continuous medium (true Gunn-Petersen effect). The mean HeII Ly-alpha opacity estimated from the depth of this depression corresponds within 1-2sigma to the values directly measured from the HI/HeII Ly-alpha forest towards the quasars studied. The observed scatter in eta = N(HeII)/N(HI) and anti-correlation between N(HI) and eta can be explained by the combined action of variable spectral softness and differences in the mean gas density between the absorbing clouds. Neither of the recovered spectral shapes show features which can be attributed to the putative input of radiation from soft sources like starburst galaxies.Comment: 20 pages, 20 figures. Accepted for publication in A&