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Objective: To compare kangaroo mother care with conventional care in newborns regarding the frequency of successful first breastfeeding and time to initiate breastfeeding. Study Design: Quasi-experimental study. Place and Duration of Study: Departments of Pediatrics and obstetrics CMH Bahawalpur from Feb 2019 to Jun 2020. Methodology: 120 infant-mother couples were included in the study. Sixty infant-mother couples were randomly allocated to each group (120 infants). Group A was nursed with kangaroo mother care (KMC), and Group B was nursed with conventional care (CC). The frequency of the first successful feed was assessed, and the time taken to initiate breastfeeding was documented. Results: There was no statistically significant difference in weight, gestational age and gender distribution between the two groups. 65 (54.25%) infants had successful first breastfeeding in the study population. 38 (63.3%) of the infants had first successful breastfeeding as per the Infant Breast feeding Assessment Tool (IBFAT) in group A (KMC) as compared to 27 (45%) in group B (Conventional Care). The difference between the two groups was statistically significant, with a p-value of 0.044. Mean time for first successful breastfeeding was significantly less for the KMC group as compared to the conventional group with a p-value of

The Deep Atmosphere Venus Investigation of Noble gases, Chemistry, and Imaging (DAVINCI) mission described herein has been selected for flight to Venus as part of the NASA Discovery Program. DAVINCI will be the first mission to Venus to incorporate science-driven flybys and an instrumented descent sphere into a unified architecture. The anticipated scientific outcome will be a new understanding of the atmosphere, surface, and evolutionary path of Venus as a possibly once-habitable planet and analog to hot terrestrial exoplanets. The primary mission design for DAVINCI as selected features a preferred launch in summer/fall 2029, two flybys in 2030, and descent sphere atmospheric entry by the end of 2031. The in situ atmospheric descent phase subsequently delivers definitive chemical and isotopic composition of the Venus atmosphere during a cloud-top to surface transect above Alpha Regio. These in situ investigations of the atmosphere and near infrared descent imaging of the surface will complement remote flyby observations of the dynamic atmosphere, cloud deck, and surface near infrared emissivity. The overall mission yield will be at least 60 Gbits (compressed) new data about the atmosphere and near surface, as well as first unique characterization of the deep atmosphere environment and chemistry, including trace gases, key stable isotopes, oxygen fugacity, constraints on local rock compositions, and topography of a tessera., Comment: 41 pages, 14 figures, accepted for publication in the Planetary Science Journal

The current study explores the impact of poverty on environmental degradation and impact of environment on poverty in the Coastal Belt of Pakistan. The poverty is measured by using headcount ratio measure. While environmental proxies used in this study are fossil fuel energy consumption from fossil fuel (FFEC), combustible waste and renewable (CRW) and carbon dioxide emission from the use of liquid fuel (CELF). The study indicates a strong long-run correlation between poverty and environmental degradation. This relationship has been investigated by using Augmented Dicky-Fuller, co-integration as well as Granger causality tests. Pakistan’s secondary data from 1971 to 2018 on poverty and environmental variables have been used for the analysis purpose. The results of the study indicate that poverty contributes to the environmental degradation and results in lowering the pace of economic growth and development. Moreover, environmental degradation also is a cause of poverty and may affect economic development adversely. The present study predicts the evidence of a bi-directional relationship between environmental factors and poverty in Pakistan.

Advances in optical testing are as important as advances in fabrication because one can make only what one can measure. A high-precision metrology capability is utilized to close the gap between interferometric testing and lower precision metrology, laser radar, or contact-probe-based coordinate measuring machines (CMM) to accurately measure surfaces with large form error. This nearly universal optical testing method employs a precision CMM equipped with a non-contact, confocal probe. This technique was developed to characterize and align a broad spectrum of optical surfaces including ones with high slopes that are nearly impossible to measure using traditional interferometric testing without custom-made optics. Optical components covering a wide range of prescriptions, such as large convex conics, high-sloped aspherics, grazing-incidence x-ray optics, and highly deformed flats, were successfully measured. The resulting data were processed using custom-developed routines to determine the optic’s alignment, the departure from design surface, and the as-built prescription parameters. This information was used to verify and guide the development and fabrication of novel optics.

Laser Induced Breakdown Spectroscopy (LIBS) in the Ultra Violet/Visible/Near-IR (UVN) spectral range is a powerful analytical tool that facilitates the interpretation of Raman spectroscopic data by providing additional details in elemental chemistry. To acquire the complete information of molecular vibrations for more accurate and precise chemical bonding and structural analysis, an ideal

The surface of ice satellites with known subsurface oceans (e.g., Europa, Ganymede, Callisto, Enceladus and Titan) are likely to contain the compositional imprints of the underlying interior ocean and their radiation processed products [1][2]. For instance, the community consensus is that Europa harbors liquid water beneath an icy crust, which has raised the possibility that life, or conditions favorable for life exist. Here we present the evolution of a powerful instrument “In situ Chemistry Experiment - μscope, Photoluminescence and Raman OBservations on Icy Satellites (ICE-μPROBIS),” a derivative of an instrument [3] proposed for a past NASA ROSES ICEE-2 AO, that can detect life biosignatures. The current Europa Lander Mission concept [4] with its advanced sample collection and analysis system, will be a blueprint for future lander/rover missions to other ocean worlds. ICE-μPROBIS instrument onboard the next generation of lander or rover mission will provide the unprecedented opportunity to carry out time-resolved Raman and photoluminescence (PL) spectroscopy, of ice samples collected from the surface, to discover if present, the types and distribution of biotic and abiotic organic compounds, measure CHNOPS containing organics and minerals and correlate them to radiolysis processed and textural features. ICE-µPROBIS includes an optical microscope to provide context imaging for the spectroscopy. Here, we describe ICE-μPROBIS’s capabilities and discuss time-resolved Raman and luminescence spectra of amino acids [5], PAHs [6] and, hydrated sulfates minerals and sulfuric acid [7] on the surface and subsurface of water-ice samples. Fig. 1. ICE-μPROBIS concept and system block diagram. ICE-µPROBIS enables in situ, spatially resolved and highly sensitive detection and characterization of organics and minerals from samples collected from icy satellite surface and near subsurface. Fig. 2. ICE-μPROBIS enables measurement of Raman spectra of the four aromatic amino acids at 5 m distance, L-phenylalanine (Phe), L-tyrosine (Tyr), L-tryptophan (Trp), L-histidine (His), and one aliphatic amino acid L-proline (Pro) [5]. Fig. 3. Standoff (120 m) TR-Raman spectra of Napthalene (PAH) inside water ice. ICE-μPROBIS will provide new insight into icy satellite surface processes by obtaining detailed analyses of surface composition. It can be used to identify key radiation products and structural changes in the sample, thus providing an indication of the extent of chemical and physical change and an estimate of the resurfaced age of the ice [6]. Fig. 4. Remote TR-Raman spectra at a distance of 5 m: a) ice nodules of 1 M sulfuric acid (H2SO4), and b) particulate ice solution of 3% hydrogen peroxide (H2O2) in distilled H2O in a lighted laboratory setting [7]. [1] Brown, M. E., et al., (2013). The Astronomical Journal, 145(4) [2] Vance, S. D., et al., (2021). Journal of Geophysical Research: Planets, 126, e2020JE006736. [3] Aslam, S., et al., (2020). AGU – iPosterSessions.com. Available online: https://www.researchgate.net/publication/346654802 [4] https://www.lpi.usra.edu/opag/meetings/opag2020fall/presentations/Hand_6014.pdf [5] Acosta-Maeda, T., (2016). Ph.D. Dissertation, https://scholarspace.manoa.hawaii.edu/bitstream/10125/51470/2016-08-phd-acostamaeda_uh.pdf [6] Sharma, S. K., et al. (2020). J. Raman Spectrosc. 51, 1782-1793. https://doi.org/10.1002/jrs.5814 [7] Sandford, M., (2020). PhD Dissertation, https://www.soest.hawaii.edu/gg/academics/theses/Sandford_Dissertation.pdf

From the Ice Giants Pre-Decadal Survey Mission Report 2017 (IGPDS), a Net Flux Radiometer (NFR) was identified in the IGPDS report as a complementary payload for a probe mission to the Ice Giants. In this paper, we will focus on the electrical architecture of an advanced NFR that is applicable to both Uranus and Neptune. The NFR contains seven spectral channels to measure energy flux from 0.2-300 μm region. The NFR rotates clockwise and anti-clockwise at 5 different viewing angles sequentially and each channel projects an unobstructed 5° field-of-view (FOV) into the atmosphere. It would enable the scientists to determine an ice giant’s atmospheric heat balance and the tropospheric 3D flow which will lead to deeper understanding the plant’s radiation, region of solar energy deposition and the atmospheric conditions [1], [2], [3], [4]. In this design, thermopile sensors are used as the detector to convert radiation energy to electrical signal. Those thermopiles are uncooled and passive detector which help to reduce overall size, weight and power (SWaP) factor of the instrument. However, the readout noise is dominated by low-frequency noise which limited the resolution of the instrument. To overcome such problem, an application specific integrated circuit (ASIC) with multi-channel analog-to-digital converter has been developed to reduce the low frequency noise of the readout system. A field-programmable-gate array (FPGA) has been integrated to the readout system to truly sample seven channels of the ASIC simultaneously. In this paper, we will go over the details of the ASIC and how to use it with the FPGA to implement the readout system for the advanced NFR. Figure 1 shows the system block diagram of the instrument [5], [6], [7]. Figure 1: System block diagram of the instrument [1] Aslam, S., et al., (2019). International Planetary Probe Workshop 2019, Oxford, UK [2] Aslam, S., et al., (2020). Space Science Reviews, 216(1) [3] Aslam, S., et al., (2018). 49th Lunar and Planetary Science Conference 2018, The Woodlands, Texas, USA, Volume: LPI Contrib. No. 2083, 2675 [4] Aslam, S., et al., (2021). EPSC Abstracts Vol. 15, EPSC2021-144, 2021 European Planetary Science Congress 2021 [5] Tran, D., et al., (2020). Sensors and Systems for Space Applications XIII 11422, 1142205. [6] Tran, D., et al., (2020). Lunar and Planetary Science Conference, 1233. [7] Quilligan, G., et al., (2021). IEEE Transactions on Nuclear Science.

We present the evolving design of an Ice-Giants Net Flux Radiometer (IG-NFR) [1][2][3], onboard a probe, Fig. 1, for in-situ measurements of the upward and downward heat flux in seven spectral channels as a function of altitude/pressure. These in situ probe measurements, will improve our understanding of energy balance and interior heat flux [4] and provide a reference profile to lift ambiguities inherent to remote observations [5]. The IG-NFR, Fig. 2, is designed to (i) accommodate seven filter bandpass channels (ii) measure up and down radiation flux in a 10° FOV for all channels in parallel; (iii) measure a change of flux of at least 0.5 W/m2 per decade of pressure; (iv) view five distinct view angles (±80°, ±45°, and 0°); (v) use application specific integrated circuit technology for the detector readout; (vii) be able to integrate radiance for 2 s or longer, and (vi) sample calibration targets every 19 s (assuming 100 m/s descent rate). Uncooled thermopile detectors are chosen for good detection sensitivity of radiation flux. A close hexagonal packing arrangement of Winston cones gives seven channels, with each Winston cone designed to give a 10° clear FOV. The Winston cone non-imaging optics, detectors and filters are all housed in a micro-vessel with CVD diamond and sapphire windows. The evacuated micro-vessel mitigates rapid excursions of temperature during the probe descent. A stepper motor with the aid of a gearbox rotates the micro-vessel, to each of the five view angles, so that the micro-vessel diamond windows have an unobstructed view through apertures in the mechanical enclosure into the atmosphere. The mechanical enclosure accommodates five apertures, hot and cold targets for radiometric calibration for each sequence of measurements (5-views). [1] Aslam, S., et al., (2018). 49th Lunar and Planetary Science Conference 2018, The Woodlands, Texas, USA, Volume: LPI Contrib. No. 2083, 2675 [2] Aslam, S., et al., (2019). International Planetary Probe Workshop 2019, Oxford, UK [3] Aslam, S., et al., (2020). Space Science Reviews, 216(1) [4] Irwin, P. G. J., et al., (2020). EPSC 2020-306, online [5] Mousis, O., et al., (2018). Planetary and Space Science 155:12-40

Icy worlds of the outer solar system contain tantalizing evidence of habitability and potential life. These bodies also present extra exploration challenges due to the harsh environmental conditions at the surfaces. Thus, robust and reliable detectors are necessary for the in situ spectroscopic identification of astrobiologically relevant compounds deposited on the icy surface, entrained in thick atmospheres, or rafted in plumes. In addition, the distinction between prebiotic, extant, and relict organic molecules in such environments is needed to address life detection goals. The Ultra-Violet Detector Innovation for Raman Exploration and CharacTerization (UV-DIRECT) of ocean worlds project focuses on the development SiC- avalanche photodiode (APD) technology for UV-Raman spectroscopy and Raman imaging. Si-based Single Photon Avalanche Diodes (SPADs) have been developed for time resolved Raman spectroscopy in recent years, but SiC (Silicon Carbide) APD detectors have advantages over them. Our detector is an ultra-compact, radiation and temperature tolerant, visible blind device that has high quantum efficiency (QE) in the DUV (~260 nm) but poorer performance in the near ultraviolet (NUV) between 300-340nm that is important for Raman Spectroscopy. Our approach to improve this combines a series of numerical models with laboratory testing to enhance the QE response and ultimately the single photon detection efficiency in the NUV (~340 nm). Raman spectroscopy has established itself in current missions as an information-rich, non-contact, non-destructive method for identifying and characterizing inorganic and organic compounds in a wide variety of planetary materials. UV/NUV-Raman spectroscopy is well-suited to characterizing plume materials and surface ice deposits, since it especially sensitive to organic compounds and inorganic salts improved sensitivity due to the combination of resonance effects and the lack of background fluorescence and less risk of sample damage compared to excitation with wavelengths Figure 1. UV-DIRECT is based on SiC-APD technology with the goal of pushing the capabilities of UV-Raman spectroscopy and Raman imaging for the exploration of icy worlds.

With the rapid advancement of imaging technology, space-based remote sensing instruments are becoming more sophisticated and are producing substantially more amounts of data for downloading. Data alteration is very likely to occur during the transmission over the long distances from probes to carrier spacecraft and subsequently back to Earth,. Cyclic Redundancy Check (CRC) is the most well-known data package error check technique which has been used in many applications. Unfortunately, due to its serial computation process, it could be a bottleneck for critical applications that require rapid processing. To overcome such issue, we present here a parallel CRC computational method based on an FPGA with simulation and testing to validate the methodology.

A portable FPM to perform wide field-of-view, high spatial-resolution imaging for biological samples is developed. An NVIDIA Jetson-Nano board is used to computationally construct the images. The FPM has the potential to be compatible to space-based payloads.

The NASA Ice Giants Pre-Decadal Survey Mission Report (2017) recommended the high scientific importance of sending a mission with an orbiter and a probe to one of the Ice Giants, with preferential launch dates in the 2029-2034 timeframe. Such a mission concept is equally well supported by European scientists and Mousis et al (P&SS, 155, 12, 2018) give compelling scientific rationales for the exploration of these worlds with missions carrying in situ probes. In this presentation we will outline the conceptual design of the Advanced Ice Giants Net Flux Radiometer (IG-NFR) instrument, currently being designed by NASA Goddard Space Flight Center to make in situ observations of the upward and downward fluxes of solar and thermal radiation in the atmospheres of Uranus and Neptune. The IG-NFR is designed to: (i) accommodate seven filter bandpass channels in the spectral range 0.25-300 µm (ii) measure up and down radiation flux in a clear unobstructed 10° FOV for each channel; (iii) use thermopile detectors that can measure a change of flux of at least 0.5 W/m2 per decade of pressure; (iv) view five distinct view angles (±80°, ±45°, and 0°); (v) predict the detector response with changing temperature environment; (vi) use application-specific integrated circuit technology for the thermopile detector readout; (vii) be able to integrate radiance for 2s or longer, and (vii) sample each view angle including calibration targets. The IG-NFR system noise equivalent power at 298 K is 73 pW in a 1 Hz electrical bandwidth. We present initial simulations of the anticipated observations using two radiative transfer and retrieval tools, NEMESIS (Irwin et al., JQSRT, 109, 1136, 2008) and the Planetary Spectrum Generator (PSG, Villanueva et al., 2017, https://psg.gsfc.nasa.gov). For the NEMESIS modelling the radiative fluxes observable at varying pressure levels were calculated with a Matrix-Operator plane-parallel multiple-scattering model, using between 5 and 21 zenith angle quadrature points and up to 38 Fourier components for the azimuth decomposition. We also employed PSG to further validate our flux estimates, providing an important benchmarking and comparison test between both models. PSG solves the scattering radiative transfer employing the discrete ordinates method, with the scattering phase function described in terms of an expansion in terms of Legendre Polynomials. Molecular cross-sections are solved via the correlated-k method employing the latest HITRAN database (Gordon et al., 2017), which are completed with the latest collision-induced-absorption (CIA, Karman et al., 2019), and UV/optical cross-sections from the MPI database (Keller-Rudek et al., 2013). For the nominal case the Sun was assumed to be at an altitude of 10° above the horizon. The internal radiance field was calculated at each internal level for a standard reference Uranus atmosphere (e.g., Irwin et al., 2017) with the addition of a single cloud layer, based at 3 bar and composed of particles with a mean radius of 1.0 µm (and size variance 0.1) and assumed complex refractive index of 1.4 + 0.001i at all wavelengths. The opacity and fractional scale height of this cloud were fitted in both models to match the combined near-infrared observations of HST/WFC3, IRTF/SpeX and VLT/SINFONI analyzed by Irwin et al. (2017). The internal radiance fields were calculated from 0.4 to 300 µm using this atmospheric model. We will show how these simulations are being used to guide the choice of spectral filter bandwidths and centres to optimize the scientific return of such an instrument. We will show that observations with such an instrument can be used to constrain effectively the radiation energy budget in the atmospheres of the Ice Giants and can also be used to determine the pressures of cloud and haze layers and broadly constrain particle size. Such modelling also allows us to simulate the visible appearance of Uranus’ atmosphere during a descent and to perform detailed validations of the simulations by comparing the two radiative transfer models (NEMESIS and PSG).

In this presentation we will describe recent work to model upward and downward fluxes of solar and thermal radiation in the atmosphere of Venus using the NEMESIS radiative transfer and retrieval tool (Irwin et al., JQSRT, 109, 1136, 2008). Using a plane-parallel matrix operator multiple-scattering model we simulate the internal 3D radiation field within Venus’ atmosphere and compare our simulations with the observations of the Pioneer Venus and Venera 13 and 14 entry probes. Such simulations allow us to assess the availability of sunlight and the visibility of the sun azimuth direction in the cloud layer for potential balloon missions, and also enables us to predict at what altitude the surface will become visible for probes descending on dayside. A reanalysis of the Venera 13 and 14 radiance spectra observations will be used to reassess earlier estimates of cloud structure and water vapour abundance. Such modelling also allows us to simulate the visible appearance of Venus’ atmosphere during the descent of a probe mission as will be shown.

NASA Goddard Space Flight Center (GSFC) has successfully developed and tested a custom-designed low-noise multi-channel digitizer (MCD) application specific integrated circuit (ASIC) for operation in harsh radiation environments. The MCD-ASIC is optimized for low-frequency and low-voltage signal measurements from sensors and transducers. It has 20 input channels where each channel is comprised of auto-zeroed chopper variable-gain amplifier, post amplifier, and a second order ΣΔ modulator. ΣΔ analog-to-digital converter (ADC) relies on oversampling and noise shaping to achieve high-resolution conversion. However, the MCD-ASIC requires digital filtering and decimation to convert the output single bit streams from the ADC to useful data words. A parallel digital platform such as a field-programmable-gate-array (FPGA) is highly suitable to fully leverage the capabilities of the MCD-ASIC. The FPGA controls the MCD-ASIC via serial peripheral interface (SPI) protocol and acquires data from it. A Python-script communicates with the FPGA board through a USB interface on a cross operating platform. Using this architecture, the system is capable of monitoring up to 20 voltage readout channels simultaneously in a real-time manner. Each channel’s parameters can be programmed independently allowing maximum user versatility. In this paper, we present analysis of the analog front-end, the implementation of the digital processing unit on the FPGA, and provide noise performance results from the MCD-ASIC readout.

A proof-of-concept, compact, portable Fourier Ptychographic Microscope (FPM) to perform wide field-of-view, high spatial resolution imaging (

The design of an advanced Net Flux Radiometer (NFR), for inclusion as a payload on a future Ice Giants probe mission, is given. The Ice Giants NFR (IG-NFR) will measure the upward and downward radiation flux (hence net radiation flux), in seven spectral bands, spanning the range from solar to far infra-red wavelengths, each with a 5° Field-Of-View (FOV) and in five sequential view angles (±80°, ±45°, and 0°) as a function of altitude. IG-NFR measurements within either Uranus or Neptune’s atmospheres, using dedicated spectral filter bands will help derive radiative heating and cooling profiles, and will significantly contribute to our understanding of the planet’s atmospheric heat balance and structure, tropospheric 3-D flow, and compositions and opacities of the cloud layers. The IG-NFR uses an array of non-imaging Winston cones integrated to a matched thermopile detector Focal Plane Assembly (FPA), with individual bandpass filters, housed in a diamond windowed vacuum micro-vessel. The FPA thermopile detector signals are read out in parallel mode, amplified and processed by a multi-channel digitizer application specific integrated circuit (MCD ASIC) under field programmable gate array (FPGA) control. The vacuum micro-vessel rotates providing chopping between FOV’s of upward and downward radiation fluxes. This unique design allows for small net flux measurements in the presence of large ambient fluxes and rapidly changing ambient temperatures during the probe descent to ≥10 bar pressure.

This white paper, written in support of NASA's 2023-2032 Planetary Decadal Survey, outlines 10 major questions that focus on the origin, evolution, and current processes that shape the atmospheres of Uranus and Neptune. Prioritizing these questions over the next decade will greatly improve our understanding of this unique class of planets, which have remained largely unexplored since the Voyager flybys. Studying the atmospheres of the Ice Giants will greatly inform our understanding of the origin and evolution of the solar system as a whole, in addition to the growing number of exoplanetary systems that contain Neptune-mass planets., Comment: 8 pages, 0 figures, White Paper submitted to the Astrobiology and Planetary Science Decadal Survey

Cash flow has been major determinant of investment in the most of the studies conducted in the area of finance. So have the studies related to financing of ships related investment projects within the maritime industry. However, the exact role of cash flow to determine the investment specially in the Maritime sector remained ambiguous. This research has been conducted mainly to investigate the relationship between investment and internal generated fund while the information is asymmetric in the Maritime and financial realms and environment of Pakistan. The Q model of investment has been used to investigate this relationship. The GMM model has been applied to test the hypothesis by using the balanced panel annual data of Pakistani listed non-financial KSE 100 index firms for the period 2009 to 2018. The empirical analysis includes 100 sample firms with 600 observations. The five measures of asymmetric information (i.e. Tobin’s Q, ownership concentration, firm size, profitability and the financial leverage) have been used in this study. The results derived by using all five measures of asymmetric information confirm the positive and statistically significant relationship between internal finance and firm’s investment when firms have information which is asymmetric in nature. This study contributes to the investment decisions in Maritime markets as well as other capital markets that are imperfect like Pakistan consisting of information asymmetries.

Raman spectroscopy and laser induced breakdown spectroscopy (LIBS) are complementary techniques that together can provide a comprehensive characterization of geologic environments. For landed missions with constrained access to target materials on other planetary bodies, discerning signatures of life and habitability can be daunting, particularly where the preservation of organic compounds that contain the building blocks of life is limited. The main challenge facing any spectroscopy measurements of natural samples is the complicated spectra that often contain signatures for multiple components, particularly in rocks that are composed of several minerals with surfaces colonized by microbes. The goal of this study was to use the combination of Raman spectroscopy and LIBS to discern different environmental regimes based on the identification of minerals and biomolecules in rocks and sediments. Iceland is a terrestrial volcano-glacial location that offers a range of planetary analog environments, including volcanically active regions, extensive lava fields, geothermal springs, and large swaths of ice-covered terrain that are relevant to both rocky and icy planetary bodies. We combined portable VIS (532 nm) and NIR (785 nm) Raman spectroscopy, VIS micro-Raman spectroscopic mapping, and UV/VIS/NIR (200 – 1000 nm) and Mid-IR (5.6 – 10 μm, 1785 – 1000 cm−1) laser induced breakdown spectroscopy (LIBS) to characterize the mineral assemblages, hydrated components, and biomolecules in rock and sediment samples collected from three main sites in the volcanically active Kverkfjoll-Vatnajokull region of Iceland: basalt and basalt-hosted carbonate rind from Hveragil geothermal stream, volcanic sediments from the base of Vatnajokull glacier at Kverkfjoll, and lava from the nearby Holuhraun lava field. With our combination of techniques, we were able to identify major mineral polytypes typical for each sample set, as well as a large diversity of biomolecules typical for lichen communities across all samples. The anatase we observed using micro-Raman spectroscopic mapping of the lava compared with the volcanic sediment suggested different formation pathways: lava anatase formed authigenically, sediment anatase could have formed in association with microbial weathering. Mn-oxide, only detected in the carbonate samples, seems to have two possible formation pathways, either by fluvial or microbial weathering or both. Even with our ability to detect a wide diversity of biomolecules and minerals in all of the samples, there was not enough variation between each set to distinguish different environments based on the limited measurements done for this study.

Multispectral snapshot imagers are capable of producing 2-D spatial images with a single exposure at selected, numerous wavelengths using the same camera, therefore, operate differently from push broom or whiskbroom imagers. They are payloads of choice in multi-angular, multi-spectral imaging missions that use small satellites flying in controlled formation, to retrieve Earth science measurements dependent on the target’s bidirectional reflectance-distribution function. Narrow fields of view are needed to capture images with moderate spatial resolution. This paper quantifies the dependencies of the imager’s optical system, spectral elements, and camera on the requirements of the formation mission and their impact on performance metrics, such as spectral range, swath, and signal-to-noise ratio (SNR). All variables and metrics have been generated from a comprehensive, payload design tool. The baseline optical parameters selected (a diameter of 7 cm, a focal length of 10.5 cm, a pixel size of $20~\mu \text{m}$ , and a field of view of 1.15°) and snapshot imaging technologies are available. The spectral components shortlisted were waveguide spectrometers, acousto-optic tunable filters (AOTF), electronically actuated Fabry–Perot interferometers, and integral field spectrographs. Qualitative evaluation favored AOTFs, because of their low weight, small size, and flight heritage. Quantitative analysis showed that the waveguide spectrometers perform better in terms of achievable swath (10–90 km) and SNR (>20) for 86 wavebands, but the data volume generated will need very high bandwidth communication to downlink. AOTFs meet the external data volume caps well as the minimum spectral (wavebands) and radiometric (SNR) requirements, therefore, are found to be currently feasible and design changes to improve swath suggested.

We describe a novel mission architecture to investigate the lower atmosphere of Saturn's moon, Titan. Titan is the only moon in the solar system to possess a dense atmosphere, which has important similarities to, and differences from, the Earth. Like Earth, Titan has lakes and seas on its surface [1] - although these are composed of liquid hydrocarbons and not water [2], [3]. The proposed mission concept is comprised of two elements: (1) A small satellite module (PCV, Probe Carrier Vehicle) that is deployed from a host Saturn system mission spacecraft, which can be a NASA small or medium class mission (either Discovery or New Frontiers mission class) and acts as a carrier and data relay for the entry probes; (2) Four atmospheric entry probes (EP), one per $\sim 10^{\mathrm{o}}$ latitude from 60-90 °N, that aerobrake and descend under parachute from $\sim 135$ km to the surface, measuring profiles of temperature, winds and gas composition during the descent. Multiple probes at different latitudes are required to constrain the spatial variation in cloud formation, precipitation and the implications for lake composition. The mission concept would require a ride-share to reach the Saturn system. Currently three of the seven anticipated New Frontiers mission destinations are in the Saturn System: Saturn Probe, Enceladus and Titan itself. The TEAM (Titan Exploration Atmospheric Microprobes) mission concept is designed to be largely independent once deployed in the Saturn system, however the prime mission spacecraft (either New Frontiers or Discovery class mission) will provide the data relay from the PCV to the Earth. Key mission challenges include thermal management and probe release and navigation.

With the rapid advancement of radiation hard imaging technology, space-based remote sensing instruments are becoming not only more sophisticated but are also generating substantially more amounts of data for rapid processing. For applications that rely on data transmitted from a planetary probe to a relay spacecraft to Earth, alteration or discontinuity in data over a long transmission distance is likely to happen. Cyclic Redundancy Check (CRC) is one of the most well-known package error check techniques in sensor networks for critical applications. However, serial CRC computation could be a bottleneck of the throughput in such systems. In this work, we design, implement, and validate an efficient hybrid look-up-table and matrix transformation algorithm for high throughput parallel computational unit to speed-up the process of CRC computation using both CPU and Field Programmable Gate Array (FPGA) with comparison of both methods.

A compact, low-noise and inexpensive preamplifier circuit has been designed and fabricated to optimally readout a common cathode (1×16) channel 4H-SiC Schottky photodiode array for use in ultraviolet experiments. The readout uses an operational amplifier with 10 pF capacitor in the feedback loop in parallel with a low leakage switch for each of the channels. This circuit configuration allows for reiterative sample, integrate and reset. A sampling technique is given to remove Johnson noise, enabling a femtoampere level readout noise performance. Commercial-off-the-shelf acquisition electronics are used to digitize the preamplifier analog signals. The data logging acquisition electronics has a different integration circuit, which allows the bandwidth and gain to be independently adjusted. Using this readout, photoresponse measurements across the array between spectral wavelengths 200 nm and 370 nm are made to establish the array pixels external quantum efficiency, current responsivity and noise equivalent power.

Credit card fraud detection has been a very demanding research area due to its huge financial implications and rampant applications in almost every area of life. Credit card fraud datasets are naturally imbalanced by having more legitimate transaction in comparison to the fraudulent transactions. Literature represents numerous studies that are aimed to balance the skewed datasets. There are two major techniques of resampling in balancing these sets i.e. under-sampling and oversampling. However both under-sampling and oversampling techniques suffer from their own set of problems that can seriously affect the performance of classifiers that have been inducted for credit card studies in the past. Thus to accelerate detection of credit card fraud, it is very important to implement the strategy that could possibly provide better predictive performance. This paper attempts to find out what resampling technique can work best under different skewed distributions for the domain of credit card fraud detection.

Here we describe the Primitive Object Volatile Explorer (PrOVE), a smallsat mission concept to study the surface structure and volatile inventory of comets in their perihelion passage phase when volatile activity is near peak. CubeSat infrastructure imposes limits on propulsion systems, which are compounded by sensitivity to the spacecraft disposal state from the launch platform and potential launch delays. We propose circumventing launch platform complications by using waypoints in space to park a deep space SmallSat or CubeSat while awaiting the opportunity to enter a trajectory to flyby a suitable target. In our Planetary Science Deep Space SmallSat Studies (PSDS3) project, we investigated scientific goals, waypoint options, potential concept of operations (ConOps) for periodic and new comets, spacecraft bus infrastructure requirements, launch platforms, and mission operations and phases. Our payload would include two low-risk instruments: a visible image (VisCAM) for 5-10 m resolution surface maps; and a highly versatile multispectral Comet CAMera (ComCAM) will measure 1) H2O, CO2, CO, and organics non-thermal fluorescence signatures in the 2-5 μm MWIR, and 2) 7-10 and 8-14 μm thermal (LWIR) emission. This payload would return unique data not obtainable from ground-based telescopes and complement data from Earth-orbiting observatories. Thus, the PrOVE mission would (1) acquire visible surface maps, (2) investigate chemical heterogeneity of a comet nucleus by quantifying volatile species abundance and changes with solar insolation, (3) map the spatial distribution of volatiles and determine any variations, and (4) determine the frequency and distribution of outbursts.

Gas Abundance Sensor Package (GASP) is a stand-alone scientific instrument that has the capability to measure the concentration of target gases based on a non-dispersive infrared sensor system along with atmospheric reference parameters. The main objective of this work is to develop a GASP system which takes advantage of available technologies and off-the-shelf components to provide a cost-effective solution for localized sampling of gas concentrations. GASP will enable scientists to study the atmosphere and will identify the conditions of the target’s planetary local environment. Moreover, due to a recent trend of miniaturization of electronic components and thermopiles detectors, a small size and robust instrument with a reduction in power consumption is developed in this work. This allows GASP to be easily integrated into a variety of small space vehicles such as CubeSats or small satellite system, especially the Micro-Reentry Capsule (MIRCA) prototype vehicle. This prototype is one of the most advanced concepts of small satellites that has the capability to survive the rapid dive into the atmosphere of a planet. In this paper, a fully-operational instrument system will be developed and tested in the laboratory environment as well as flight preparation for a field test of the instrument suite will be described.

In 1995, the Galileo spacecraft arrived at Jupiter to conduct follow-up experiments on pathfinder Pioneer and key Voyager discoveries especially at Io, Europa, Ganymede and Callisto. These new observations helped expand our scientific knowledge of the prominent Galilean satellites; studies revealed diversity with respect to their geology, internal structure, evolution and degree of past and present activity. Jupiter's diverse Galilean satellites, of which three are believed to harbor internal oceans, are central to understanding the habitability of icy worlds. Galileo provided for the first time compelling evidence of a near-surface global ocean on Europa. Furthermore, by understanding the Jupiter system and unraveling the history of its evolution from initial formation to the emergence of possible habitats and life, gives insight into how giant planets and their satellite systems form and evolve. Most important, new light is shed on the potential for the emergence and existence of life in icy satellite oceans. In 2009, NASA released a detailed Jupiter Europa Mission Study (EJSM) that proposed an ambitious Flagship Mission to understand more fully the satellites Europa and Ganymede within the context of the Jovian system. Key to EJSM is the NASA led Jupiter Europa Orbiter (JEO) and the ESA led Jupiter Ganymede Orbiter (JGO). JEO and JGO would execute a choreographed exploration of the Jovian system before settling into orbit around Europa and Ganymede, respectively. The National Academies Planetary Decadal Survey, 2011 has listed the NASA-led JEO as the second highest priority mission for the decade 2013-2022, and if chosen it would be launched in 2020 with arrival at Jupiter in 2025. If the JEO mission is not chosen it is anticipated that there will be opportunities in future decadal cycles. Jupiter Orbit Insertion (JOI) begins a 30-month Jovian system tour followed by nine months of science mapping after Europa Orbit Insertion (EOI) in July 2028. The orbiter will ultimately impact the surface of Europa after the mission is completed. The current JEO mission concept includes a range of instruments on the payload, to monitor dynamic phenomena (such as Io's volcanoes and Jupiters atmosphere), map the Jovian magnetosphere and its interactions with the Galilean satellites, and characterize water oceans beneath the ice shells of Europa and Ganymede. The payload includes a low mass (3.7 Kg) and low power (< 5 W) Thermal Instrument (TI) concept for measuring possible warm thermal anomalies on Europa s cold surface caused by recent (< 10,000 years) eruptive activity. Regions of anomalously high heat flow will be identified by thermal mapping using a nadir pointing, push-broom filter radiometer that provides far-IR imagery in two broad band spectral wavelength regions, 8-20 m and 20-100 m, for surface temperature measurements with better than a 2 K accuracy and a spatial resolution of 250 m/pixel obtained from a 100 Km orbit. The temperature accuracy permits a search for elevated temperatures when combined with albedo information. The spatial resolution is sufficient to resolve Europa's larger cracks and ridge axial valleys. In order to accomplish the thermal mapping, the TI uses sensitive thermopile arrays that are readout by a custom designed low-noise Multi-Channel Digitizer (MCD) ASIC that resides very close to the thermopile linear array outputs. Both the thermopile array and the MCD ASIC will need to show full functionality within the harsh Jovian radiation environment, operating at cryogenic temperatures, typically 150 K to 170 K. In the following, a radiation mitigation strategy together with a low risk Radiation-Hardened-By-Design (RHBD) methodology using commercial foundry processes is given for the design and manufacture of a MCD ASIC that will meet this challenge.

A SiN membrane based MgB2 thin-film bolometer, with a non-optimized absorber, has been fabricated that shows an electrical noise equivalent power of 256 fW/square root Hz operating at 30 Hz in the 8.5 - 12.35 micron spectral bandpass. This value corresponds to an electrical specific detectivity of 7.6 x 10(exp 10) cm square root Hz/W. The bolometer shows a measured blackbody (optical) specific detectivity of 8.8 x 10(exp 9) cm square root Hz/W, with a responsivity of 701.5 kV/W and a first-order time constant of 5.2 ms. It is predicted that with the inclusion of a gold black absorber that a blackbody specific detectivity of 6.4 x 10(exp 10) cm/square root Hz/W at an operational frequency of 10 Hz, can be realized for integration into future planetary exploration instrumentation where high sensitivity is required in the 17 - 250 micron spectral wavelength range.

The composite infrared spectrometer (CIRS) instrument on board the Cassini Saturn orbiter employs two 1x10 HgCdTe detector arrays for mid-infrared remote sensing of Titan's and Saturn's atmospheres. In this paper we show that the real detector spatial response functions, as measured in ground testing before launch, differ significantly from idealized "boxcar" responses. We further show that neglecting this true spatial response function when modeling CIRS spectra can have a significant effect on interpretation of the data, especially in limb-sounding mode, which is frequently used for Titan science. This result has implications not just for CIRS data analysis but for other similar instrumental applications.