Fibrodysplasia Ossificans Progressiva -Second Skeleton

For my poster presentation, I chose how disease, illness, and sickness are defined differently in medicine. Specifically, the humanities bring awareness to treating the person as a whole rather than their prognosis. The ability to differentiate the aforementioned criteria allows for the individual to have the best treatment and outcome. I decided to show how within Fibrodysplasia Ossificans Progressiva (FOP) there are different definitions of the diagnosis. The poster delves into the definition of disease as the medical definition of the diagnosis—essentially, what the doctor informs to the patient. With FOP, common characteristic of the disease include stiff rigidity of the shoulders and neck, the inability to walk, and randomized flare-ups that cause painful calcified growths muscles and tissues that surrounds the skeleton. Illness is how the individual experiences their own prognosis. Jasmin Floyd is an activist who, through social media, has brought awareness to FOP and how she has learned to live with the terminal diagnosis. Sickness is how society has stigmatized the diagnosis. Flare-ups due to FOP cause people to look different than others. Creating a hurdle that may not have been addressed in the disease diagnosis as something an individual has to think of. How will society view me? Comments like mannequin and statue are a few examples of the negative connotations used. To conclude, the humanities in health care bring awareness to treating the person as a whole rather than their prognosis. Having the ability to differentiate the aforementioned criteria allows for the individual to have the best treatment and outcome. skeleton, FOP, disease, illness, sicknesshttps://digitalcommons.misericordia.edu/research_posters2021/1000/thumbnail.jp

Use of CT to Diagnose Subcutaneous Emphysema (SE)

Subcutaneous emphysema is a follow up symptom to a traumatic event, surgery, or nose-blowing. In addition subcutaneous emphysema is considered benign and self limiting. Computed tomography (CT) is the imaging modality of choice for diagnosing subcutaneous emphysema. CT is preferred because of its sensitivity to tissue densities. A CT will demonstrate dark air pockets within the subcutaneous layer of the skin. Furthermore, upon palpation of the the skin a crepitus crackling sound is demonstrated. Moreover, listening to the skin with a stethoscope will emit a high-frequency acoustic sound. Nevertheless, extensive subcutaneous emphysema may require medical assistance. Typically, orbital subcutaneous emphysema is non-life threatening and will resolve within a few days as the body absorbs the air. If the air is extensive and compresses on the optic nerve medical attention is required to prevent vision loss. In addition, traumatic subcutaneous emphysema may be caused from pneumothorax or other blunt trauma. The air rises and spreads within the body and can travel though different anatomical planes. Lastly, subcutaneous emphysema may be a complication of surgical procedures. Individuals are susceptible to suffering from subcutaneous emphysema after procedures like colonoscopies. To conclude, subcutaneous emphysema is a symptom that can be diagnosed by CT and is relatively harmless. Keywords: Subcutaneous emphysema, CT, benign, crepitushttps://digitalcommons.misericordia.edu/medimg_seniorposters/1032/thumbnail.jp

FLAGCAL:A flagging and calibration package for radio interferometric data

We describe a flagging and calibration pipeline intended for making quick look images from GMRT data. The package identifies and flags corrupted visibilities, computes calibration solutions and interpolates these onto the target source. These flagged calibrated visibilities can be directly imaged using any standard imaging package. The pipeline is written in "C" with the most compute intensive algorithms being parallelized using OpenMP.Comment: 15 Pages, 6 figures, 2 Tables, Accepted for publication in the Experimental Astronomy Journa

“Pockets of Hope”: Changing Representations of Diversity in Newbery Medal–Winning Titles

Newbery Medal–winning books provide cultural models for children’s developing cultural understandings of themselves and others. This article presents results of a critical content analysis that used sociocultural and historical lenses to examine representations of race/ethnicity, gender, and ability of main characters across the Newbery-winning corpus and how these representations have changed over the history of the award, 1922–2019. Findings present a lack of consistent diverse representation across all fields, with increased diverse representation in the most recent decades. The discussion contextualizes findings against historical events. Understanding the representations of diversity in these texts and the historical contexts within which such texts have emerged provides grounding to problematize the status quo of the curriculum and suggests a need for critical questioning and grand conversations

Magnification Effects on Source Counts and Fluxes

We consider the effect of lensing magnification on high redshift sources in the case that magnification varies on the sky, as expected in wide fields of view or within observed galaxy clusters. We give expressions for number counts, flux and flux variance as integrals over the probability distribution of the magnification. We obtain these through a simple mapping between averages over the observed sky and over the magnification probability distribution in the source plane. Our results clarify conflicting expressions in the literature and can be used to calculate a variety of magnification effects. We highlight two applications: 1. Lensing of high-z galaxies by galaxy clusters can provide the dominant source of scatter in SZ observations at frequencies larger than the SZ null. 2. The number counts of high-z galaxies with a Schechter-like luminosity function will be changed at high luminosities to a power law, with significant enhancement of the observed counts at L > 10 L*.Comment: 5 pages, 2 figures; accepted for publication in MNRA

Bright Source Subtraction Requirements For Redshifted 21 cm Measurements

The \hi 21 cm transition line is expected to be an important probe into the cosmic dark ages and epoch of reionization. Foreground source removal is one of the principal challenges for the detection of this signal. This paper investigates the extragalactic point source contamination and how accurately bright sources ($\gtrsim 1$ ~Jy) must be removed in order to detect 21 cm emission with upcoming radio telescopes such as the Murchison Widefield Array (MWA). We consider the residual contamination in 21 cm maps and power spectra due to position errors in the sky-model for bright sources, as well as frequency independent calibration errors. We find that a source position accuracy of 0.1 arcsec will suffice for detection of the \hi power spectrum. For calibration errors, 0.05 % accuracy in antenna gain amplitude is required in order to detect the cosmic signal. Both sources of subtraction error produce residuals that are localized to small angular scales, \kperp \gtrsim 0.05 Mpc$^{-1}$, in the two-dimensional power spectrum.Comment: 12 pages, 19 Figures, submitted to Ap

Angular 21 cm Power Spectrum of a Scaling Distribution of Cosmic String Wakes

Cosmic string wakes lead to a large signal in 21 cm redshift maps at redshifts larger than that corresponding to reionization. Here, we compute the angular power spectrum of 21 cm radiation as predicted by a scaling distribution of cosmic strings whose wakes have undergone shock heating.Comment: 13 pages, 6 figures; v2: minor modifications, journal versio

How well can we measure and understand foregrounds with 21 cm experiments?

Before it becomes a sensitive probe of the Epoch of Reionization, the Dark Ages, and fundamental physics, 21 cm tomography must successfully contend with the issue of foreground contamination. Broadband foreground sources are expected to be roughly four orders of magnitude larger than any cosmological signals, so precise foreground models will be necessary. Such foreground models often contain a large number of parameters, reflecting the complicated physics that governs foreground sources. In this paper, we concentrate on spectral modeling (neglecting, for instance, bright point source removal from spatial maps) and show that 21 cm tomography experiments will likely not be able to measure these parameters without large degeneracies, simply because the foreground spectra are so featureless and generic. However, we show that this is also an advantage, because it means that the foregrounds can be characterized to a high degree of accuracy once a small number of parameters (likely three or four, depending on one's instrumental specifications) are measured. This provides a simple understanding for why 21 cm foreground subtraction schemes are able to remove most of the contaminants by suppressing just a small handful of simple spectral forms. In addition, this suggests that the foreground modeling process should be relatively simple and will likely not be an impediment to the foreground subtraction schemes that are necessary for a successful 21 cm tomography experiment.Comment: 15 pages, 9 figures, 2 tables; Replaced with accepted MNRAS version (slight quantitative changes to plots and tables, no changes to any conclusions

Lensing Magnification: Implications for Counts of Submillimeter Galaxies and SZ Clusters

We study lensing magnification of source galaxies by intervening galaxy groups and clusters using a halo model. Halos are modeled with truncated NFW profiles with ellipticity added to their lensing potential and propagated to observable lensing statistics. We present the formalism to calculate observable effects due to a distribution of halos of different masses at different redshifts along the l ine of sight. We calculate the effects of magnification on the number counts of high-redshift galaxies. Using BLAST survey data for submillimeter galaxies (SMGs), we find that magnification affects the steep, high flux par t of the counts by about 60%. The effect becomes much stronger if the intrinsic distribution is signi ficantly steeper than observed. We also consider the effect of this high-redshift galaxy population on contaminating the Sunyaev-Zel'dovich (SZ) signal of massive clusters using the halo model approach. We find that for the majority of clusters expected to be detected with ongoing SZ surveys, there is significant contamination from the Poisson noise due to background SMGs. This contr ibution can be comparable to the SZ increment for typical clusters and can also contaminate the SZ decrement of low mass clusters. Thus SZ observations, especially for the increment part of the SZ spectrum, need to include careful modeling of this irreducible contamination for mass estimation. Lensing further enhances the contamination, especially close to the cores of massive clusters and for very disturbed clusters with large magnification cross-section.Comment: 21 pages, 14 figures, Submitted to MNRA

Redshift Space Distortion of the 21cm Background from the Epoch of Reionization I: Methodology Re-examined

The peculiar velocity of the intergalactic gas responsible for the cosmic 21cm background from the epoch of reionization and beyond introduces an anisotropy in the three-dimensional power spectrum of brightness temperature fluctuations. Measurement of this anisotropy by future 21cm surveys is a promising tool for separating cosmology from 21cm astrophysics. However, previous attempts to model the signal have often neglected peculiar velocity or only approximated it crudely. This paper presents a detailed treatment of the effects of peculiar velocity on the 21cm signal. (1) We show that properly accounting for finite optical depth eliminates the unphysical divergence of 21cm brightness temperature in the IGM overdense regions found in previous work that employed the usual optically-thin approximation. (2) We show that previous attempts to circumvent this divergence by capping the velocity gradient result in significant errors in the power spectrum on all scales. (3) We further show that the observed power spectrum in redshift-space remains finite even in the optically-thin approximation if one properly accounts for the redshift-space distortion. However, results that take full account of finite optical depth show that this approximation is only accurate in the limit of high spin temperature. (4) We also show that the linear theory for redshift-space distortion results in a ~30% error in the power spectrum at the observationally relevant wavenumber range, at the 50% ionized epoch. (5) We describe and test two numerical schemes to calculate the 21cm signal from reionization simulations which accurately incorporate peculiar velocity in the optically-thin approximation. One is particle-based, the other grid-based, and while the former is most accurate, we demonstrate that the latter is computationally more efficient and can achieve sufficient accuracy. [Abridged