readily be attributed to the choice of abundances used in the spectral fitting. With in three of the four years. These indicate a long term periodicity on the range of these new NH values, along with new Av values from Balmer decrement years and some shorter term periodicity in the range of months, consistent with observations, we can recalculate the slope of the linear relation. As this relation is what was expected. Period analysis has been done on the data and preliminary commonly used to help constrain the distance to X-ray sources, subtle changes in results will be presented. We will keep observing this system to see if there is this relation can have important consequences for a variety of astrophysical further evidence of long term periodicity and to see if the monthly variations applications. continue.

523.02 – Finding Short-Term Variability in Methanol Masers 523.06 – The HETG Orion Legacy Project: Abundances in Trapezium Stars 1 1 1 2 2 Samuel Bonin1, W. C. Barott2, T. Catanach3 Norbert S. Schulz , D. P. Huenemoerder , N. Shen , P. Testa , J. Nichols , C. R. 1 1University of New Mexico, 2Embry-Riddle Aeronautical University, 3University of Canizares Notre Dame. 1MIT, 2CfA. 9:00 AM - 2:00 PM 9:00 AM - 2:00 PM The Allen Telescope Array (ATA) performed 53 observations of 6.7 GHz methanol The ONC is an ideal astrophysical laboratory to study very young stars. The HETG masers between July 2010 and January 2011 in an effort to identify short-timescale Orion Legacy Project is designed to obtain a large number of high-resolution X-ray variability. With the notable exception of Weisberg et al. (2005), few analyses have spectra of very young late type pre-main sequence stars, and several young been performed analyzing variability in masers on timescales of minutes or less. massive and intermediate mass stars. Its extreme proximity and youth makes the This work is aimed both at providing additional data (including refined positions) core of the ONC a Chandra legacy project involving the only high resolution on the catalog of observed sources as well as identifying the prevalence and cause spectroscopic study of young embedded cluster stars for decades to come. For of short-term phenomena. Observations utilized both the ATA correlator (for several PMS stars we derive abundance fractions from temperature-insensitive line mapping) and beamformer (for recording voltage time series). A combination of ratios. From these fractions we construct a single abundance distribution involving Fast-Fourier Transforms and Continuous Wavelet Transforms are applied to O, Mg, Ne, Si, S, Ar, and Fe to fit all X-ray spectra simultaneously. We compare this channelized power series waterfalls) in this investigation. Wavelet analysis can be common abundance distribution to abundances determined recently in more thought of as a generalization of Fourier analysis that allows us to examine massive Orion Trapezium stars and to results from several other abundance non-stationary characteristics of the spectra. The survey included both short (10 studies of Orion stars and clusters. minute), long (60 minute), and follow-up observations on candidate targets. Analysis so far has identified three variable sources out of 43 distinct objects that 523.07 – Weak Emission Lines in the NIR Spectrum of 3 Cen A were observed. These objects exhibit significant variation on the order of several Glenn Michael Wahlgren1, M. F. Nieva2, N. Przybilla2 minutes, are consistent in follow-up observations, and we have ruled out 1 2 instrumental variation. Future and ongoing work includes identifying the source of NASA-HQ/CUA, Univ. Erlangen-Nuremberg, Germany. this variation as intrinsic to the source or a property of the ISM. Shorter 9:00 AM - 2:00 PM time-scales will be investigated using a combination of techniques, including total Infrared spectral observations of the chemically peculiar star 3 Cen A (B5p) have power variation, pulse searching (in an attempt to find pulsars), and phase-shift been made as part of the CRIRES-POP program to observe bright stars at high demodulation techniques. The case for SETI analysis of these data is given, for spectral resolution using the ESO/VLT/CRIRES instrument. The program has been example, by Cordes (1993), who suggested that extraterrestrial intelligences could described by Lebzelter et al (2012, A&A, 539, 109). Here, we discuss the detection use masers to amplify interstellar signals.This project was funded by the National of weak emission lines (WELs) arising from singly-ionized elements, including P, Science Foundation Grant AST0852095. [1] Weisberg J. M. et al. (2005) Science, Mn, and Fe. The emission lines at IR wavelengths complement the emission lines 309, 5731. [2] Cordes J. M. (1993) Astron. Soc. Pacific Conf. Series, 47, 257. catalogued for this star at optical wavelengths (Wahlgren & Hubrig, 2004, A&A, 418, 1073). We aim to extend the system of energy levels associated with WELs to 523.03 – Abundances in Red Giant Stars in IC 4756 higher energy to identify the mechanism of their creation. We have performed Julie Djordjevic1, J. King1 NLTE modeling at optical and NIR wavelengths for several species. Early results from modeling of Fe II shows that NLTE effects can be large and in a manner that 1Clemson University. improves the synthetic spectrum fit of the observations compared with LTE 9:00 AM - 2:00 PM synthetic spectrum modeling. We present high-resolution spectroscopy of red giant stars in the open cluster IC 4756 from the McDonald Observatory 2.1m. Results include relative abundance 523.08 – Complex Scattered Radiation Fields And Multiple Magnetic Fields measurements as well as stellar atmospheric parameters. This work is supported In The Protostellar Cluster In NGC 2264 by NSF grant AST 09-08342 to JRK. The observations were originally supported by Jungmi KWON1, M. Tamura1, R. Kandori2, N. Kusakabe2, J. Hashimoto2, Y. NASA through the grant HF-1046.01-93A to JRK from the Space Telescope Science 2 2 3 4 5 6 Institute, which is operated by the Association of Universities for Research in Nakajima , F. Nakamura , T. Nagayama , T. Nagata , J. H. Hough , M. W. Werner , Astronomy, Inc. under NASA Contract No.NAS 5-26555. P. S . Te i x e i r a 7 1NAOJ/GUAS, Japan, 2NAOJ, Japan, 3Nagoya University, Japan, 4Kyoto University, 523.04 – XMM-Newton And Chandra Observations Of The Galactic Mixed- 5 6 morphology Supernova Remnant G352.7-0.1 Japan, University of Hertfordshire, United Kingdom, Jet Propulsion Laboratory, 7 Thomas Pannuti1, J. P. Napier1 California Institute of Technology, European Southern Observatory, Germany. 9:00 AM - 2:00 PM 1Morehead State University. 9:00 AM - 2:00 PM Near-infrared imaging polarimetry in the J, H, and Ks bands has been carried out for the protostellar cluster region around NGC 2264 IRS 2 in the Monoceros OB1 We present an analysis of pointed archival X-ray observations made with molecular cloud. Various infrared reflection nebula clusters (IRNCs) associated XMM-Newton and Chandra of the Galactic mixed-morphology supernova remnant with NGC 2264 IRS 2 and the IRAS 12 S1 core, as well as local infrared reflection (SNR) G352.7-0.1. Mixed-morphology SNRs feature a shell-like radio morphology nebulae (IRNe), were detected. The illuminating sources of the IRNe were with a contrasting center-filled thermal morphology: the origin of the contrasting identified with known or new near- and mid-infrared sources. In addition, 314 morphologies observed for these sources is not well-understood, thus necessitating point-like sources were detected in all three bands and their aperture polarimetry further study of these remarkable objects. Previous X-ray observations made of this was studied. Using a color-color diagram, reddened field stars and diskless SNR have revealed the presence of an ejecta-dominated plasma with enhanced pre-main-sequence stars were selected to trace the magnetic field structure of the elemental abundances of silicon and sulfur) along with a remarkably high molecular cloud. The mean polarization position angle of the point-like sources is temperature of approximately kT ~ 2 keV. We present a spatially-resolved ~80 degrees in the cluster core, and ~60 degrees in the perimeter of the cluster spectroscopic study of this emission to search for spectral and spatial variations in core, which is interpreted as the projected direction on the sky of the magnetic the X-ray-emitting plasma: we also conduct a search for a neutron star. Initial field in the observed region of the cloud. The Chandrasekhar-Fermi method gives a results will be presented and discussed. rough estimate of the magnetic field strength to be about 100 micro-Gauss. A comparison with recent numerical simulations of the cluster formation implies that 523.05 – Optical Monitoring and Period Analysis of High Mass X-Ray Binary the cloud dynamics is controlled by the relatively strong magnetic field. The local System BD+53 2262 magnetic field direction is well associated with that of CO outflow for IRAS 12 S1 1 1 Nathaly Zurita , E. G. Hintz and consistent with that inferred from submillimeter polarimetry. In contrast, the 1Brigham Young University. local magnetic field direction runs roughly perpendicular to the Galactic magnetic 9:00 AM - 2:00 PM field direction. High mass X‐ray binary systems (HMXB) are usually composed of a B spectral type 523.09 – The Photometric Period and Variability of the Cataclysmic Variable star and a neutron star. These systems have been primarily observed in the X‐ray V849 Herculis (PG 1633+115) regime and as such their optical properties have not been thoroughly studied. We 1 1 1 1 hypothesize that variability/periodicity in the optical brightness should be present Fred Ringwald , G. D. Rude, II , J. J. Roveto , K. K. Khamvongsa and correlate with variability at other wavelengths. For the last five summers, 1California State University, Fresno. optical observations of HMXB system BD+53 2262 have been gathered on the 9:00 AM - 2:00 PM David Derrick 16’’ telescope located at Brigham Young University. To probe for We report time-resolved photometry of the cataclysmic variable V849 Her, and long‐term and short term variability, observations were taken in quick succession measure a period of 0.1414 ± 0.0030 days (3.394 ± 0.072 h). We also present in one filter over the course of a night and also shorter observations through photometry taken over several weeks in 2010 and 2011, as well as light curves multiple filters spaced over many nights. The observations are primarily in the from 1995 to 2011 by the American Association of Variable Star Observers. The Johnson V filter, with B and I added in 2010, and R in 2011. We present optical spectra, absolute magnitude derived from infrared magnitudes, and variability all light curves for five years of observations of the system BD+53 2262. There is a suggest that V849 Her is a nova-like variable. The shallow (0.5-magnitude) low definite decrease in magnitude in the past five years and small monthly variations states we observe resemble the erratic low states of the VY Sculptoris stars, although they may recur quasi-periodically over an average cycle of 12.462 ± supported by the Helmholtz Association through the research alliance “Planetary 0.074 days. Evolution and Life“.

523.1 – Warm H2O And OH Disk Emission In 1548c27 523.14 – Probing the Circumstellar Environment of the Herbig Ae Star MWC Greg Doppmann1, J. Najita2, J. Carr3 325 1 2 3 4 5 1W. M. Keck Observatory, 2NOAO, 3NRL. Sam Ragland , K. Ohnaka , L. Hillenbrand , S. T. Ridgway , M. M. Colavita , R. 9:00 AM - 2:00 PM Akeson6, W. Cotton7, W. C. Danchi8, M. Hrynevych1, R. Millan-Gabet6, W. A. Traub5 Circumstellar disks are fundamentally important in the formation of stars and 1W. M. Keck Observatory, 2Max-Planck-Institut für Radioastronomie, Germany, planets, and high resolution L-band spectra provide an essential tool for 3California Institute of Technology, 4National Optical Astronomy Observatories, characterizing the inner disk region (< 1AU) around young stars where 5 6 terrestrial-like planets may form. By extending our modeling technique developed Jet Propulsion Laboratory, California Institute of Technology, NExScI, California 7 8 for fitting the disk emission features in V1331 Cyg, we model the broad water and Institute of Technology, National Radio Astronomy Observatory, NASA Goddard OH emission that is observed in the probable Herbig AeBe star, 1548C27, from our Space Flight Center, Exoplanets and Stellar Astrophysics. NIRSPEC/Keck L-band spectra (R=24,000). We use the HITEMP line list to model 9:00 AM - 2:00 PM the water emission in 1548C27, which gives an improved fit to V1331 Cyg We present the first N-band nulling plus K- and L-band squared-visibility compared with models using the BT2 list. When compared to V1331 Cyg, the water observations of a young stellar object, MWC 325, taken with the 85 m baseline and OH model fits to 1548C27 reveal (1) similarly high temperatures (T ~ 1500K), Keck Interferometer. Interferometric observations of MWC 325 at K, L and N indicating that the emission originates from the inner disk, (2) similarly high encompass a factor of five in spectral range and thus, especially when spectrally columns of OH and water (N ~ 1021–1022 cm-2), suggesting a deeper temperature dispersed within each band, enable characterization of the structure of the inner -1 disk regions where planets form. Fitting our observations with geometric models inversion in the disk atmosphere, and (3) rapid disk rotation (vsini > 60 km s ), such as a uniform disk or a Gaussian disk show that the apparent size increases indicating a more edge-on disk orientation along our line-of-sight. monotonically with wavelength in the 2-12 micron wavelength region, confirming the widely held assumption based on radiative transfer models, now with spatially 523.11 – Hidden Gems: Resolving M/L Dwarf + T Dwarf Binaries 1 2 resolved measurements over broad wavelength range, that disks are extended with Christopher R. Gelino , A. J. Burgasser a temperature gradient. The existing interferometric measurements and the 1Caltech, 2UCSD. spectral energy distribution can be reproduced by a flat disk or a weakly-shadowed 9:00 AM - 2:00 PM nearly flat-disk model, with only slight flaring in the outer regions of the disk, The multiplicity properties of very low mass stars and brown dwarfs are critical consisting of representative "sub-micron" and "micron" grains of a 50:50 ratio of empirical constraints for formation theories, while multiples themselves provide silicate and graphite. This is marked contrast with the disks previously found in unique opportunities to test evolutionary and atmospheric models and examine other Herbig Ae/Be stars suggesting a wide variety in the disk properties among empirical trends. Existing samples of late-type binaries are drawn almost entirely Herbig Ae/Be stars. from resolved imaging programs, limiting our understanding of the closely- separated binary population for which dynamical mass measurements and transit 523.15 – The Core Velocity Dispersion (CVD) for Taurus Dense Core Clusters observations are most likely. We have developed a method for identifying and Di Li1, L. Qian2 characterizing unresolved, late-type M/L dwarf + T dwarf binaries using 1California Institute of Technology, 2National Astronomical Observatories, China. low-resolution, near-infrared spectroscopy, a method that is not constrained by 9:00 AM - 2:00 PM separation limitations. We have obtained high resolution imaging with Keck NIRC2 We define a statistical measurement--Core Velocity Dispersion (CVD) for the LGS-AO for approximately 30 candidate binaries identified by this method. In this dynamics of a dense core cluster. To obtain a well defined CVD requires a poster we characterize the most widely-separated, resolved systems and set limits spectroscopic dense core sample located in a contiguous region. We measure CVD on the separations of unresolved systems. The former provide necessary for Taurus cores utilizing the ~100 d^2 13CO map corrected for depletion. The information for characterizing the still poorly-understood L dwarf/T dwarf Taurus CVD has the same power law as that of the Larson's law. No sign of transition and the first epochs for astrometric orbit determinations; the latter are additional energy input is seen. optimal targets for high resolution, spectroscopic monitoring.

523.16 – Understanding Star Formation in the Rosette Molecular Complex: 523.12 – Photometric and Spectroscopic Analysis of Eclipsing Binary TY Tau A Chandra View of the Embedded Young Clusters Jennifer Wojno1, C. H. S. Lacy2 Junfeng Wang1 1University of Louisville, 2University of Arkansas. 1Harvard-Smithsonian CfA/SAO. 9:00 AM - 2:00 PM 9:00 AM - 2:00 PM We have used photometric observations collected from November 2000 to The Rosette Molecular Cloud (RMC) complex represents an ideal laboratory for December 2010 using the 10" URSA telescope at the University of Arkansas as well understanding star formation processes, and we have carried out a Chandra as spectroscopic observations from other sources of the eclipsing binary system TY imaging survey of the embedded clusters to characterize the young stellar Tau to determine the relative radii, mass, and luminosities of the stars in the populations. We present new X-ray results on the embedded young star cluster system. These results suggest that this system consists of on ZAMS or near-ZAMS RMC PL6 and in particular the massive young stellar object AFGL 961, which is early K star and a companion which has not yet reached the ZAMS. The solution previously resolved in the near-infrared (the Rosette Eye, Li et al. 2008). also suggests that there may be a third member of this system, although we cannot exclude contamination by an external source from these observations. Further observations of this system may refine the ages of these stars, and also determine 523.17 – Spectropolarimetry and Type Ia Supernovae 1 1 whether there is a distant third member of this system or whether the residual flux Amber L. Porter , M. Leising is due to an unrelated object. 1Clemson University. 9:00 AM - 2:00 PM 523.13 – Two Different Sources of Water in Earth’s Accretion Zone of the Spectropolarimetry of Type Ia supernovae sheds lights on the asymmetric Solar Nebula outermost geometry of these cataclysmic events. Non-zero polarization detections 1 1 1 1 Ekkehard Kuehrt , C. Tornow , S. Kupper , P. Gast hint at a roughly spherical photosphere enveloped in ejected material with the 1DLR-German Aerospace Center, Germany. supernova becoming more spherical with time as we see deeper into the ejecta. 9:00 AM - 2:00 PM Further study is needed to determine the nature of the asymmetry, among possibilities such as clumping or non-spherical ejection. We investigate how a The origin of water and the related significance for the early Earth depend on the supernova’s ejecta velocity distribution is correlated to the polarization of certain conditions in the different stages of the solar nebula and the later solar system. spectral features for different origins of asymmetry. With our model we simulate the chemical and hydrodynamic processes of the solar nebula. For that purpose we explicitly consider the evolution of the parental cloud core, its gravitational collapse, and the resulting turbulent disk. As a consequence 523.18 – The Properties and Kinematics of a New Sample of Cool Subdwarfs of the low temperature (~8 K) in the center of the cloud core thick ice layers are from SDSS 1 1 2 formed on the dust grains. The collapse is simulated using a new semi-analytic Antonia Savcheva , A. A. West , J. Bochanski multi-zone solution of the hydrodynamic equations which is valid for spherical 1Boston Univ., 2Pennsylvania State University. symmetry. Initially, the density distribution of the inner zone represents a central 9:00 AM - 2:00 PM clump from which the proto-sun and later the T Tauri Sun form. The two outer We present a sample of 2114 M subdwarfs from the 7th Data Release of the Sloan zones evolve into a disk and a thin but spatially extended envelope. The disk stage Digital Sky Survey (DR7; SDSS). This catalog contains stellar coordinates, SDSS is described by a stationary model and considers a weakly coupled gas and dust magnitudes, spectral classes, radial velocities, proper motions, absolute phase. We have identified two different sources of water for the region of Earth’s magnitudes and estimated distances. We discuss the selection criteria, the spectral accretion. The first source is located in the inner region of the collapsing cloud classification and radial velocity determination processes. We calculate 3D space core where the temperature could reach about 500 K. There, water was produced motions (U,V,W) in the standard Galactic system and place each star in its proper efficiently by gas phase reactions between neutral molecules. The second source is subdwarf subclass (as defined by Lepine et al.). We show that the metal poor related to icy mantles of dust grains formed in the cloud core and disk stage. In the populations are moving faster than the metal rich stars on average, consistent with course of disk evolution cooling caused an enrichment of the dust phase with water being members of a dynamically heated thick disk or halo population. In addition, ice beyond the snowline which moved inwards, i.e. into the Earth accretion zone. we present two different versions of the reduced proper motion (RPM) diagram, In addition we present results how water formation is related to the initial including a new formulation of the classic RPM diagram that includes information abundance ratio between carbon and oxygen in the cloud. This research has been about the radial velocity. We discuss a few curious subsets of our sample, including