DOCSLIB.ORG

Undergraduate Research Symposium May 21, 2010 Mary Gates Hall Online Proceedings

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Undergraduate Research Symposium May 21, 2010 Mary Gates Hall Online Proceedings Undergraduate Research Symposium May 21, 2010 Mary Gates Hall Online Proceedings Silicon Nanophotonic Waveguides for the Mid-Infrared POSTER SESSION 1 Alexander Weber (Alexander) Spott, Senior, Electrical Balcony, Easel 134 Engineering, Mathematics (Comprehensive) Mary Gates Scholar 12:00 PM to 1:00 PM Andrew Weber (Andrew) Spott, Senior, Physics In Situ Calibration of Magnetic Probes in a Flux Mary Gates Scholar Conserver Mentor: Michael Hochberg, Electrical Engineering Cosmo Lucas (Cosmo) Smith, Senior, Physics, Computer It has been demonstrated that silicon nanophotonic waveg- Science, English (Creative Writing) uides can be used to construct all of the components of a pho- Mary Gates Scholar, NASA Space Grant Scholar tonic data transmission system on a single chip. Complex Mentor: Simon Woodruff, Woodruff Scientific electro-photonic integrated circuits can be constructed from With an exponentially increasing global population, the ne- the integration of nanophotonic waveguides and CMOS elec- cessity of finding renewable and sustainable energy sources tronics. It has also been shown that the high field confinement is becoming unavoidable. Plasma fusion provides a highly of silicon nanoscale guides enables a variety of new applica- promising, virtually inexhaustible and environmentally be- tions, including chip-scale nonlinear optics, as well as biosen- nign energy source by using particles heated to over 100 mil- sors and light-force activated devices. Currently, the majority lion degrees Celsius to run a power plant. Fusion is still in de- of experiments with silicon waveguides have been at wave- velopment, however, due to a number of technical difficulties, lengths in the near-infrared, between 1.1-2 µm. Our research chief among which is confinement and sustainment of the su- demonstrates that by using a material system which lacks a perheated particles, also known as plasma. In the analysis of high index substrate, single-mode silicon nano-waveguides confined plasma, magnetic inductive probes are essential for can be used at mid-infrared wavelengths, in particular at 4.5 their ability to reveal information about plasma shape, posi- µm, or 2222.2 cm−1. This idea has appeared in theoretical tion and current density without physically interacting with literature, but experimental realization has been elusive. This the plasma. Magnetic inductive probes are vital to sphero- result represents the first practical integrated waveguide sys- maks – devices used to contain plasma - for real-time control tem for the mid-infrared in silicon, and enables a range of of the plasma along with reconstruction of its equilibrium. new applications. The magnetic diagnostic system in our experiment includes 50 probes embedded in the surface of a copper flux conserver surrounding the plasma. These probes are arranged in 25 POSTER SESSION 1 probe-pairs that measure both toroidal and poloidal magnetic MGH 241, Easel 180 fields. Due to attenuation effects on the magnetic field by the 12:00 PM to 1:00 PM copper, the probes on the flux conserver must be calibrated in situ. This is accomplished by performing two simulations in Model of Chromosome Movement During Cell Division which a toroidal and a poloidal field are independently gen- Suggests that a Viscoelastic Linkage Coordinates Paired erated. By testing at several different frequencies, the attenu- Sister Chromatids ation effect on the magnetic probes can be characterized and Carol Jessica Huseby, Senior, Physics, Biology (Physiology) the probes can be accurately calibrated. Proper calibration is NASA Space Grant Scholar a necessary step towards precise plasma measurements and, Mentor: Charles Asbury, Physiology and Biophysics ultimately, towards an understanding of how confined plas- Mentor: Anton Andreev mas can be sustained. Birth defects and cancers can occur if the genetic material in cells, the DNA, is not segregated properly during cell divi- POSTER SESSION 1 sion. Replicated DNA is packaged into joined chromosome pairs, called ‘sisters’, which make attachments to the tips of Balcony, Easel 123 microtubule filaments through specialized structures, called 12:00 PM to 1:00 PM kinetochores. Sister kinetochore pairs then make oscillatory movements driven by the stochastic lengthening and shorten- Undergraduate Research Program 1 exp.washington.edu/urp ing of the microtubules to which they are attached. To explain how the movements of sisters are coordinated, a ‘push-pull’ POSTER SESSION 1 model has been proposed where the dynamics of kinetochore- Commons West, Easel 70 attached filaments are regulated by forces transmitted through 12:00 PM to 1:00 PM the packaged DNA that links the sisters together. Here we show that the simplest version of this model, in which the An Examination of K-12 Teacher Understanding of linkage is assumed to be purely elastic, fails in computer sim- Limits in the Context of Kinematics ulations to reproduce the near-perfect coordination of sisters Alexis Rebecca Werner (Alexis) Olsho, Fifth Year, Physics seen in cells. Furthermore, by tracking sister kinetochores in NASA Space Grant Scholar high-resolution movies of live cells, we find that the prob- Mentor: Peter Shaffer, Physics ability for a kinetochore to reverse direction correlates not Mentor: MacKenzie Stetzer, Physics only with the distance separating it from its sister, but also The Physics Education Group (PEG) in the Physics Depart- with the direction that its sister is moving. The latter im- ment at the University of Washington is involved in research, plies that microtubules attached to one kinetochore somehow curriculum development, and instruction aimed at improving ‘sense’ whether those attached to the sister kinetochore are student learning in physics. Part of the work involves helping growing or shrinking. This effect, and the highly coordinated prepare K-12 teachers of physics and physical science. To movement of sisters observed in cells, can be reproduced in this end, the group is developing an inquiry-based curricu- computer simulations assuming the sisters are connected with lum, Physics by Inquiry (PbI), designed to strengthen subject a material in which its effective stiffness can change with the matter background in physics and physical science. I worked rate of sister separation. We therefore propose that sister kine- at the 2009 NSF Summer Institute for Inservice Teachers, an tochore movements during cell division are coordinated by intensive 5-week program that used the PbI curriculum. I in- inter-kinetochore forces transmitted through viscoelastic ma- vestigated participant conceptual understanding of mathemat- terial between sisters. ical limits primarily in the context of kinematics, as well as in the context of electric circuits. The project began by con- POSTER SESSION 1 ducting a detailed examination of pretests and post-tests from Commons West, Easel 53 previous summers. These indicated that many K-12 teachers are unable to use limiting procedures when presented with 12:00 PM to 1:00 PM information in non-graphical form. By developing additional Sharing the Sky: Using Social Technologies for Scientific pretests and post-tests that were administered to the 2009 par- Collaboration ticipants, we gained insight into participant understanding be- Ian Michael (Ian) Smith, Junior, Physics, Astronomy fore, during, and after instruction. The in-depth analysis of Mentor: Andrew Connolly, Astronomy participant responses throughout the summer helped us as- sess the effectiveness of the PbI curriculum in kinematics in As enormous amounts of data are collected by the large mul- general, with a particular focus on the teaching of limit con- tispectral survey programs such as Sloan Digital Sky Sur- cepts in the context of velocity and acceleration. This detailed vey (SDSS), and soon the Large Synoptic Survey Telescope analysis of the prevalence of various types of errors has pro- (LSST), we are faced with the challenge of finding a way to vided a deeper understanding of the difficulties that teachers meaningfully interact with this data to maximize scientific face when learning the material, is guiding the further de- return. Our goal is to create a flexible environment that or- velopment of curriculum, and is contributing to the existing ganizes disparate data sources, such as streamed images and research base on the learning and teaching of physics. database services, to be analyzed visually through the coordi- nation of simple tools that work on common data. We envi- sion a framework that allows users to personalize their access POSTER SESSION 1 to data and to easily create custom tools to interact with and Commons West, Easel 72 import data from new sources. The web browser is a natural 12:00 PM to 1:00 PM place to create such an environment, and by leveraging the OpenSocial API we extend our model to allow collaboration A High-Power 556nm Source for Laser Cooling of between astronomers remotely. In addition to enhancing ac- Ytterbium Atoms cess to data among astronomers, the web application will be Jiawen Pi, Senior, Physics available to the public, encouraging exploration of the sky. Mentor: Subhadeep Gupta, Physics Mentor: Vladyslav Ivanov, Physics The fine structure constant is a fundamental scientific quan- tity because it characterizes the strength of the fundamental 2 interaction between light and matter. Cold ytterbium (Yb) tified as BAL QSOs in SDSS and we subsequently observe atoms are promising candidates for accurate measurements them with FAST across 3 consecutive nights, and then on day of this constant using atom interferometry techniques. It is 9, 27, and 81. Additional observations are acquired for 1 and possible to cool Yb atoms to temperatures of few micro- 2 year cadences. We also obtain a set of control non-BAL Kelvin using coherent laser radiation. This is achieved by us- quasar spectra, in which we expect to see little or no variabil- ing laser cooling, where atomic motion is cooled by counter- ity. We assess the magnitude of the variability in the observed propagating resonant laser light at 556nm (green), a wave- spectra of our BAL QSOs and determine which constraints length not easily reachable by common laser sources.
Load more

Recommended publications
  • Planets and Exoplanets
    NASE Publications Planets and exoplanets Planets and exoplanets Rosa M. Ros, Hans Deeg International Astronomical Union, Technical University of Catalonia (Spain), Instituto de Astrofísica de Canarias and University of La Laguna (Spain) Summary This workshop provides a series of activities to compare the many observed properties (such as size, distances, orbital speeds and escape velocities) of the planets in our Solar System. Each section provides context to various planetary data tables by providing demonstrations or calculations to contrast the properties of the planets, giving the students a concrete sense for what the data mean. At present, several methods are used to find exoplanets, more or less indirectly. It has been possible to detect nearly 4000 planets, and about 500 systems with multiple planets. Objetives - Understand what the numerical values in the Solar Sytem summary data table mean. - Understand the main characteristics of extrasolar planetary systems by comparing their properties to the orbital system of Jupiter and its Galilean satellites. The Solar System By creating scale models of the Solar System, the students will compare the different planetary parameters. To perform these activities, we will use the data in Table 1. Planets Diameter (km) Distance to Sun (km) Sun 1 392 000 Mercury 4 878 57.9 106 Venus 12 180 108.3 106 Earth 12 756 149.7 106 Marte 6 760 228.1 106 Jupiter 142 800 778.7 106 Saturn 120 000 1 430.1 106 Uranus 50 000 2 876.5 106 Neptune 49 000 4 506.6 106 Table 1: Data of the Solar System bodies In all cases, the main goal of the model is to make the data understandable.
    [Show full text]
  • Doppler Tomography of the Circumstellar Disk of Π Aquarii⋆⋆⋆
    A&A 560, A30 (2013) Astronomy DOI: 10.1051/0004-6361/201322114 & c ESO 2013 Astrophysics Doppler tomography of the circumstellar disk of π Aquarii, S. V. Zharikov1, A. S. Miroshnichenko2 , E. Pollmann3, S. Danford2,K.S.Bjorkman4, N. D. Morrison4,A.Favaro5, J. Guarro Fló6,J.N.Terry7, V. Desnoux8, T. Garrel9, G. Martineau10, Y. Buchet10, S. Ubaud11, B. Mauclaire12, H. Kalbermatten13,C.Buil14,C.J.Sawicki15,T.Blank16, and O. Garde17 1 Observatorio Astronomico Nacional, Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, 22800 Ensenada, BC, Mexico e-mail: [email protected] 2 University of North Carolina at Greensboro, Greensboro, NC 27402, USA e-mail: [email protected] 3 Emil-Nolde-Str. 12, 51375 Leverkusen, Germany 4 Ritter Observatory, University of Toledo, Toledo, OH 43606, USA 5 19 Boulevard Carnot, 21000 Dijon, France 6 Balmes, 2, 08784 Piera (Barcelona), Spain 7 6 rue Virgile, 42100 Saint-Etienne, France 8 ARAS, Astronomical Ring for Access to Spectroscopy, France 9 Observatoire de Juvignac, 19 avenue du Hameau du Golf, 34990 Juvignac, France 10 SAPP, CSC des Trois Cités, Le Clos Gaultier, 86000 Poitiers, France 11 16 Calade, St. Roch, 06410 Biot, France 12 Observatoire du Val de l’Arc, route de Peynier, 13530 Trets, France 13 Ebnetstrasse 12, Bitsch, Switzerland 14 Castanet Tolosan Observatory, 6 place Clémence Isaure, 31320 Castanet Tolosan, France 15 Alpha Observatory, Alpine, Texas 79830, USA 16 Dorfstrasse 3f, 8603 Schwerzenbach, Switzerland 17 Observatoire de la Tourbiére, 38690 Chabons, France Received 21 June 2013 / Accepted 23 October 2013 ABSTRACT Aims. The work is aimed at studying the circumstellar disk of the bright classical binary Be star π Aqr.
    [Show full text]
  • 00E the Construction of the Universe Symphony
    The basic construction of the Universe Symphony. There are 30 asterisms (Suites) in the Universe Symphony. I divided the asterisms into 15 groups. The asterisms in the same group, lay close to each other. Asterisms!! in Constellation!Stars!Objects nearby 01 The W!!!Cassiopeia!!Segin !!!!!!!Ruchbah !!!!!!!Marj !!!!!!!Schedar !!!!!!!Caph !!!!!!!!!Sailboat Cluster !!!!!!!!!Gamma Cassiopeia Nebula !!!!!!!!!NGC 129 !!!!!!!!!M 103 !!!!!!!!!NGC 637 !!!!!!!!!NGC 654 !!!!!!!!!NGC 659 !!!!!!!!!PacMan Nebula !!!!!!!!!Owl Cluster !!!!!!!!!NGC 663 Asterisms!! in Constellation!Stars!!Objects nearby 02 Northern Fly!!Aries!!!41 Arietis !!!!!!!39 Arietis!!! !!!!!!!35 Arietis !!!!!!!!!!NGC 1056 02 Whale’s Head!!Cetus!! ! Menkar !!!!!!!Lambda Ceti! !!!!!!!Mu Ceti !!!!!!!Xi2 Ceti !!!!!!!Kaffalijidhma !!!!!!!!!!IC 302 !!!!!!!!!!NGC 990 !!!!!!!!!!NGC 1024 !!!!!!!!!!NGC 1026 !!!!!!!!!!NGC 1070 !!!!!!!!!!NGC 1085 !!!!!!!!!!NGC 1107 !!!!!!!!!!NGC 1137 !!!!!!!!!!NGC 1143 !!!!!!!!!!NGC 1144 !!!!!!!!!!NGC 1153 Asterisms!! in Constellation Stars!!Objects nearby 03 Hyades!!!Taurus! Aldebaran !!!!!! Theta 2 Tauri !!!!!! Gamma Tauri !!!!!! Delta 1 Tauri !!!!!! Epsilon Tauri !!!!!!!!!Struve’s Lost Nebula !!!!!!!!!Hind’s Variable Nebula !!!!!!!!!IC 374 03 Kids!!!Auriga! Almaaz !!!!!! Hoedus II !!!!!! Hoedus I !!!!!!!!!The Kite Cluster !!!!!!!!!IC 397 03 Pleiades!! ! Taurus! Pleione (Seven Sisters)!! ! ! Atlas !!!!!! Alcyone !!!!!! Merope !!!!!! Electra !!!!!! Celaeno !!!!!! Taygeta !!!!!! Asterope !!!!!! Maia !!!!!!!!!Maia Nebula !!!!!!!!!Merope Nebula !!!!!!!!!Merope
    [Show full text]
  • Arxiv:1402.5240V1 [Astro-Ph.SR]
    Accepted in ApJ A Preprint typeset using LTEX style emulateapj v. 04/17/13 DISK-LOSS AND DISK-RENEWAL PHASES IN CLASSICAL BE STARS. II. CONTRASTING WITH STABLE AND VARIABLE DISKS Zachary H. Draper1,2, John P. Wisniewski3, Karen S. Bjorkman4, Marilyn R. Meade5, Xavier Haubois6,7, Bruno C. Mota6, Alex C. Carciofi6, Jon E. Bjorkman4 Accepted in ApJ ABSTRACT Recent observational and theoretical studies of classical Be stars have established the utility of polarization color diagrams (PCD) in helping to constrain the time-dependent mass decretion rates of these systems. We expand on our pilot observational study of this phenomenon, and report the detailed analysis of a long-term (1989-2004) spectropolarimetric survey of 9 additional classical Be stars, including systems exhibiting evidence of partial disk-loss/disk-growth episodes as well as sys- tems exhibiting long-term stable disks. After carefully characterizing and removing the interstellar polarization along the line of sight to each of these targets, we analyze their intrinsic polarization be- havior. We find that many steady-state Be disks pause at the top of the PCD, as predicted by theory. We also observe sharp declines in the Balmer jump polarization for later spectral type, near edge-on steady-state disks, again as recently predicted by theory, likely caused when the base density of the disk is very high, and the outer region of the edge-on disk starts to self absorb a significant number of Balmer jump photons. The intrinsic V -band polarization and polarization position angle of γ Cas exhibits variations that seem to phase with the orbital period of a known one-armed density structure in this disk, similar to the theoretical predictions of Halonen & Jones.
    [Show full text]
  • 108 Afocal Procedure, 105 Age of Globular Clusters, 25, 28–29 O
    Index Index Achromats, 70, 73, 79 Apochromats (APO), 70, Averted vision Adhafera, 44 73, 79 technique, 96, 98, Adobe Photoshop Aquarius, 43, 99 112 (software), 108 Aquila, 10, 36, 45, 65 Afocal procedure, 105 Arches cluster, 23 B1620-26, 37 Age Archinal, Brent, 63, 64, Barkhatova (Bar) of globular clusters, 89, 195 catalogue, 196 25, 28–29 Arcturus, 43 Barlow lens, 78–79, 110 of open clusters, Aricebo radio telescope, Barnard’s Galaxy, 49 15–16 33 Basel (Bas) catalogue, 196 of star complexes, 41 Aries, 45 Bayer classification of stellar associations, Arp 2, 51 system, 93 39, 41–42 Arp catalogue, 197 Be16, 63 of the universe, 28 Arp-Madore (AM)-1, 33 Beehive Cluster, 13, 60, Aldebaran, 43 Arp-Madore (AM)-2, 148 Alessi, 22, 61 48, 65 Bergeron 1, 22 Alessi catalogue, 196 Arp-Madore (AM) Bergeron, J., 22 Algenubi, 44 catalogue, 197 Berkeley 11, 124f, 125 Algieba, 44 Asterisms, 43–45, Berkeley 17, 15 Algol (Demon Star), 65, 94 Berkeley 19, 130 21 Astronomy (magazine), Berkeley 29, 18 Alnilam, 5–6 89 Berkeley 42, 171–173 Alnitak, 5–6 Astronomy Now Berkeley (Be) catalogue, Alpha Centauri, 25 (magazine), 89 196 Alpha Orionis, 93 Astrophotography, 94, Beta Pictoris, 42 Alpha Persei, 40 101, 102–103 Beta Piscium, 44 Altair, 44 Astroplanner (software), Betelgeuse, 93 Alterf, 44 90 Big Bang, 5, 29 Altitude-Azimuth Astro-Snap (software), Big Dipper, 19, 43 (Alt-Az) mount, 107 Binary millisecond 75–76 AstroStack (software), pulsars, 30 Andromeda Galaxy, 36, 108 Binary stars, 8, 52 39, 41, 48, 52, 61 AstroVideo (software), in globular clusters, ANR 1947
    [Show full text]
  • The Comet's Tale and (Spacewatch), 1998 M5 Need of Observation
    THE COMET’S TALE Newsletter of the Comet Section of the British Astronomical Association Volume 6, No 2 (Issue 12), 1999 October THE SECOND INTERNATIONAL WORKSHOP ON COMETARY ASTRONOMY New Hall, Cambridge, 1999 August 14 - 16 After months of planning and much hard work the participants for the second International Workshop on Cometary Astronomy began to assemble at New Hall, Cambridge on the afternoon and evening of Friday, August 13th. New Hall is one of the more recent Cambridge colleges and includes a centre built for Japanese students as well as accommodation for the graduate and undergraduate students. It is a women’s college and a few participants were later disturbed by the night porter doing his rounds and making sure that all ground floor windows were closed. A hearty dinner was provided, but afterwards I had to leave to continue last minute preparations for the morning. He had searched 1000 hours since Most discoveries were from On Saturday morning, Dan Green 1994 without a discovery. If the Japan, USA and Australia. and Jon Shanklin made a few Edgar Wilson award had been in Southern Hemisphere observers opening announcements. We had operation he would have netted an only discover southern declination nine comet discoverers present average of $4000 a year, though comets, however northern and five continents were some years would be more hemisphere observers find them in represented. The next meeting rewarding and others less. His both hemispheres. There is no would take place in 4 – 5 years search technique is to scan significant trend in discovery time, possibly in America.
    [Show full text]
  • Polarimetry of Early Emission Line Stars
    UvA-DARE (Digital Academic Repository) Polarimetry of Early Emission Line Stars. McDavid, D. Publication date 2001 Link to publication Citation for published version (APA): McDavid, D. (2001). Polarimetry of Early Emission Line Stars. General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:28 Sep 2021 Chapterr 4 Multicolorr Polarimetry of Selected Be Stars: 1990-93 3 (originallyy published in 1994 PASP, 106, 949) ABSTRACT T Opticall polarization data in the XJBVRI filter system for eight bright northernn Be stars are presented here as the continuation of a long term mon- itoringg project begun in 1984. There are no strong cases of night-to-night variability,, and the only star showing unmistakable changes in polarization fromfrom year to year over the nine years covered by the program is Pi Aquarii.
    [Show full text]
  • Disk Loss and Disk Renewal Phases in Classical Be Stars I: Analysis of Long-Term Spectropolarimetric Data
    Accepted in ApJ Dec 8, 2009 A Preprint typeset using L TEX style emulateapj v. 11/12/01 DISK LOSS AND DISK RENEWAL PHASES IN CLASSICAL BE STARS I: ANALYSIS OF LONG-TERM SPECTROPOLARIMETRIC DATA John P. Wisniewski1,2, Zachary H. Draper1, Karen S. Bjorkman3, Marilyn R. Meade4, Jon E. Bjorkman3, Adam F. Kowalski1 Accepted in ApJ Dec 8, 2009 ABSTRACT Classical Be stars are known to occasionally transition from having a gaseous circumstellar disk (“Be phase”) to a state in which all observational evidence for the presence of these disks disappears (“normal B-star phase”). We present one of the most comprehensive spectropolarimetric views to date of such a transition for two Be stars, π Aquarii and 60 Cygni. 60 Cyg’s disk loss episode was characterized by a generally monotonic decrease in emission strength over a time-scale of ∼1000 days from the maximum V-band polarization to the minimum Hα equivalent width, consistent with the viscous time-scale of the disk, assuming α ∼0.14. π Aqr’s disk loss was episodic in nature and occurred over a time-scale of ∼2440 days. An observed time lag between the behavior of the polarization and Hα in both stars indicates the disk clearing proceeded in an “inside-out” manner. We determine the position angle of the intrinsic polarization to be 166.7±0.1◦ for π Aqr and 107.7±0.4◦ for 60 Cyg, and model the wavelength dependence of the observed polarization during the quiescent diskless phase of each star to determine the interstellar polarization along the line of sight.
    [Show full text]
  • Undergraduate Research Symposium May 21, 2010 Mary Gates Hall Online Proceedings
    Undergraduate Research Symposium May 21, 2010 Mary Gates Hall Online Proceedings POSTER SESSION 1 POSTER SESSION 1 MGH 241, Easel 178 Balcony, Easel 115 12:00 PM to 1:00 PM 12:00 PM to 1:00 PM The Role of the Mitotic Kinase Plk1 and the AKAP Trace-Contaminant Degradation by Wastewater Gravin in Cellular Transformation Microorganisms Karly Anne (Karly) Fischer, Senior, Biology (Physiology) Wayne Tamell (Wayne) Mc Neal, Senior, Civil Engineering Mentor: John Scott, Pharmacology NASA Space Grant Scholar, McNair Scholar Mentor: David Canton, Pharmacology, Howard Hughes Mentor: Heidi Gough, Civil And Environmental Engineering Medical Institute Mentor: John Ferguson, Civil And Environmental Engineering Propagation of cellular signals through protein phosphoryla- tion and dephosphorylation are key regulatory mechanisms in Trace-level contaminants originating from pharmaceuticals mammalian cells. Perturbation of these signaling pathways and personal care products (PPCP) represent a new class can lead to numerous disease states, including cancer. These of contaminants which are suspected to cause adverse im- molecules and their interaction partners are integral parts of pacts to aquatic life. These compounds often enter aquatic every physiological system. Our interest in the regulation of systems through sewers systems and wastewater treatment cellular signaling through the action of a family of proteins plants. The identification of organisms capable of degrad- known as A-kinase anchoring proteins (AKAPs) is important. ing PPCP will contribute greatly to the design and imple- AKAPs are signal-organizing molecules that bind to cyclic- mentation of new processes for the removal of PPCP dur- AMP-dependent protein kinase A (PKA) to further propagate ing wastewater treatment.
    [Show full text]
  • Volume 28 (Pdf)
    title page go es here Be Star Newsletter Contents Editorial A New Lo ok G J Peters The Electronic Journal D R Gies Working Group Matters WG to meet in the Hague D R Gies Contributions A Recent Emission Episo de of Lambda Eri S Ste A Simulation of NRP and Prole Variability D R Gies and M E Hahula Velocity Variations Asso ciated with Nonradial Pulsation D Gies H Observations of Kappa Dra and Kappa CMa J Hao Whats Happ ening Observing Campaign on Lambda Eri R Hirata Observing Campaign on Ostars H Henrichs Hot Star Newsletter P Eenens Preprints Received NearIR variability of Be stars S M Dougherty and A R Taylor NearIR excess of Be stars S M Dougherty et al Tomographic Separation of Comp osite Sp ectra I I I UV Detection of the Hot Companion of Phi Persei M L Thaller et al Multicolor Polarimetry of Selected Be Stars D McDavid Bibliography Be stars B stars Meetings ASTROPHYSICAL APPLICATIONS OF STELLAR PULSATION Note to Subscrib ers How to obtain the pap er version of the Newsletter Be Star Newsletter EDITORIAL A New Lo ok Greetings from a new editorial team and to a new lo ok for the Be Star Newsletter As mentioned in the last issue of the Newsletter the SOC of the Working Group on Be Stars has recommended that
    [Show full text]
  • Three Small Super-Earths Transiting the Nearby Star GJ 9827
    Accepted for publication in AJ on October 25, 2017 Preprint typeset using LATEX style AASTeX6 v. 1.0 THREE SUPER-EARTHS TRANSITING THE NEARBY STAR GJ 9827 Prajwal Niraula1, Seth Redfield1, Fei Dai2,3, Oscar Barragan´ 4, Davide Gandolfi4, P. Wilson Cauley1, Teruyuki Hirano5, Judith Korth6, Alexis M. S. Smith7, Jorge Prieto-Arranz8,9, Sascha Grziwa6, Malcolm Fridlund10,11, Carina M. Persson11, Anders Bo Justesen12, Joshua N. Winn2, Simon Albrecht12, William D. Cochran13, Szilard Csizmadia7, Girish M. Duvvuri1, Michael Endl13, Artie P. Hatzes14, John H. Livingston15, Norio Narita15,16,17, David Nespral8,9, Grzegorz Nowak8,9, Martin Patzold¨ 6, Enric Palle8,9, and Vincent Van Eylen10 1Astronomy Department and Van Vleck Observatory, Wesleyan University, Middletown, CT 06459, USA; [email protected] 2Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA 3Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 4Dipartimento di Fisica, Universit´adi Torino, via P. Giuria 1, 10125 Torino, Italy 5Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan 6Rheinisches Institut f¨urUmweltforschung an der Universit¨atzu K¨oln,Aachener Strasse 209, 50931 K¨oln,Germany 7Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, 12489 Berlin, Germany 8Instituto de Astrof´ısicade Canarias, C/ V´ıaL´acteas/n, 38205 La Laguna, Spain 9Departamento
    [Show full text]
  • The COLOUR of CREATION Observing and Astrophotography Targets “At a Glance” Guide
    The COLOUR of CREATION observing and astrophotography targets “at a glance” guide. (Naked eye, binoculars, small and “monster” scopes) Dear fellow amateur astronomer. Please note - this is a work in progress – compiled from several sources - and undoubtedly WILL contain inaccuracies. It would therefor be HIGHLY appreciated if readers would be so kind as to forward ANY corrections and/ or additions (as the document is still obviously incomplete) to: [email protected]. The document will be updated/ revised/ expanded* on a regular basis, replacing the existing document on the ASSA Pretoria website, as well as on the website: coloursofcreation.co.za . This is by no means intended to be a complete nor an exhaustive listing, but rather an “at a glance guide” (2nd column), that will hopefully assist in choosing or eliminating certain objects in a specific constellation for further research, to determine suitability for observation or astrophotography. There is NO copy right - download at will. Warm regards. JohanM. *Edition 1: June 2016 (“Pre-Karoo Star Party version”). “To me, one of the wonders and lures of astronomy is observing a galaxy… realizing you are detecting ancient photons, emitted by billions of stars, reduced to a magnitude below naked eye detection…lying at a distance beyond comprehension...” ASSA 100. (Auke Slotegraaf). Messier objects. Apparent size: degrees, arc minutes, arc seconds. Interesting info. AKA’s. Emphasis, correction. Coordinates, location. Stars, star groups, etc. Variable stars. Double stars. (Only a small number included. “Colourful Ds. descriptions” taken from the book by Sissy Haas). Carbon star. C Asterisma. (Including many “Streicher” objects, taken from Asterism.
    [Show full text]