A Pharmacogenomic and Protein Analysis of Human Lacrimal Fluid in Varying Age Groups

Proteins are large biological molecules located within all cells. They are considered the basic functional components of cells that allow them to operate appropriately. Genes consist of both DNA and RNA, and are the cellular components that code for the proteins. A biomarker is any cellular component that is an indication of a biological state. Therefore, genetic and protein biomarkers are specific genes and proteins, respectively, present in cells that indicate a specific biological state of a cell. Identification of proteins and genetic biomarkers in relative quantities has been found to reflect various disease states and age groups in humans. Comparisons of possible techniques for collecting lacrimal fluids from human subjects which could potentially be utilized in the design of the study

Protein Analysis of Human Lacrimal Fluid in Varying Age Groups

Purpose: The objective of this research project was to identify proteins secreted from human lacrimal fluids onto the extra-ocular surface of the eye that could be later used to predict eye health, disease, and age-related changes. The identification of specific lacrimal proteins in relative quantities and patterns in younger versus older patients may reflect both ocular and extra-ocular disease states. Methods: This observational study collected samples of lacrimal fluid from 20 subjects between the ages of 18 and 25 years and 20 subjects over the age of 50 years with the use of Schirmer strips. The protein composition of these lacrimal fluid samples was then analyzed to determine specific proteins that evidenced unique patterns among the subject populations. Results: The protein concentrations between the two age groups (n = 40) was significantly higher in the younger patient group (1408.3 ug/mL versus 1152.5 ug/mL, p = 0.03). No consistent qualitative differences in the protein bands were observed between the two different patient age groups. However, excising and analyzing the outlying protein bands revealed unique proteins within the older patient group (aldehyde dehydrogenase and serotransferrin precursor). Preliminary attempts were made to determine the presence of proteins in lacrimal fluid that may originate from cells lining the ducts and blood vessels associated with the ocular environment. Conclusion: These preliminary results in age related differences in eye lacrimal fluid will contribute to future research endeavors in order to determine which specific proteins were increased or decreased quantitatively in the younger population, if any, and what role they might have in eye health, disease, and age-related changes

Multi-messenger observations of a binary neutron star merger

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40+8-8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Mo. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One- Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta

Multi-messenger Observations of a Binary Neutron Star Merger

International audienceOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta