Lumbar Drain Monitor — Biomedical Instrumentation & Clinical Sensing

Abstract — Lumbar Drain Monitor

stacks, simulation worlds, reports and viva from Bangalore. We use galaxies detected in a deep ultraviolet XMM- Newton Optical Monitor image and a model that predicts UV galaxy counts based on local counts and evolution pa- rameters to constrain galaxy evolution to Z=1.2. The 17’ square 2000 IA (UVW2 Ilter) image was taken as part of tect sources in this image to a Iux limit of 2.7 × 10−17 ergs cm−2 s−1 IA−1 (AB magnitude = 22). Since some of the sources may be stars, we perform a number of checks, in- cluding shape, color and implied distance to remove stars from the detected counts. We Ind galaxy number counts as a function of magnitude roughly in agreement Milliard et al. (1992), but again Ind these counts are in excess of evolution models. The excess counts at faint magni- tudes may provide evidence for either a new population of galaxies emerging around Z=0.7 or more dramatic evo- lution than some earlier predictions. The integrated light from the detected galaxies totals 32–36 ph cm−2 s−1 IA−1 sr−1, placing a Irm lower limit on the integrated UV light from galaxies.

Sensor Interfacing & Analog Front-End Conditioning

Measurements of the integrated light from a galaxy at 2000 IA provides a fairly direct measure of the instanta- neous rate of star formation, since the massive stars that provide most of this radiation are short-lived compared with the age of the galaxy. Knowledge of the star forma- tion rate also gives a measure of the rate of heavy element production in a galaxy, or in the universe when a large sample of galaxies are measured (Madau et al. 1996). The integrated light from these galaxies contributes to the ex- tragalactic background light at ultraviolet wavelengths, whose main sources are hot stars and active galactic nu- clei. Measurements of galaxy number counts in the ultra- violet have been made by Milliard et al. (1992) using the FOCA balloon-borne UV telescope, Gardner et al. (2000) and Hill et al. (1997) using HST archival Ields. These data have been interpreted with models that predict num- ber counts based on galaxy spectral energy distributions (SED’s) and luminosity functions, such as those of Ar- mand & Milliard (1994) and Granato et al. (2000). The to- tal far-ultraviolet extragalactic background has been mea- sured to be as high as 500 ph cm−2 s−1 IA−1 and as low as 30 ph cm−2 s−1 IA−1 (see review by Bowyer 1991). Predic- tions for the number of galaxies that might be detected in deep ultraviolet Optical Monitor (OM) images are given by Sasseen et al. (1997). In this paper, we detect galaxies in a deep UV image taken with the Optical Monitor (OM) and use these galaxy number counts to place constraints on galaxy luminosity evolution via a a galaxy evolution model similar to that of Armand & Milliard (1994). We also Ind a lower limit to the galaxy contribution to the extragalactic UV background.

Bio-Signal Waveform Analysis & Simulation Findings

The OM 13 hr deep Ield (at J2000.0 13 34 37.00, +37 54 44.0) was observed for approximately 200 ks with XMM- Newton around June 22, 2001. Details of the OM expo- sures used in this study are shown in Table 1. Several exposures of typically 7 ks were brought to a common astrometric reference frame and coadded. We searched each image for sources using Sextractor and made a catalog of the sources we found. We concentrate here on sources in the UVW2 image (Fig. 1) and use measure- ments in the other Ilters to diIerentiate between stars, galaxies and QSO’s. We also use a deep R band image (to R∼27) of this Ield taken with the 8m Subaru tele- scope on Mauna Kea (Fig. 2) to check for source shape and possible confusion. We perform two checks to discrim- Proc. Symposium ‘New Visions of the X-ray Universe in the XMM-Newton and Chandra Era’ against stellar templates. Second, we compute an inferred distance, as if the source were a main sequence star, from U-B color and B magnitude, as shown in Fig. 3. We Ind these checks form reliable stellar discriminators for more than 90% of the sources brighter than AB=22. 1 We also Ind a number of QSO’s in the Ield that show UV excess and appear point-like in the OM and Subaru images. We categorize these separately in our galaxy number counts.

Scope & Clinical Applications

• Real-time multi-parameter vital signs telemetry (ECG, Heart Rate, SpO2, Temperature, Respiration)
• Low-noise Analog Front-End (AFE) conditioning with active Driven Right Leg (DRL) 50 Hz cancellation
• Digital signal processing in MATLAB: Pan-Tompkins QRS detection, FIR/IIR notch, and Continuous Wavelet Transforms
• Finite element tissue bio-electromagnetics and orthopedic mechanical simulations in COMSOL & ANSYS
• Complete Arduino firmware .INO sketches, circuit schematics, and university dissertation reports