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2017EGUGA..1915045L

The knowledge of sea level height is important for many different sectors as navigation transport building infrastructures tourism or maritime sports between others. Tides are mainly composed of an astronomical part and a meteorological one. Sometimes their joined action is the responsible of extreme behaviors in the sea level. Influence of pressure differences as well as related winds is important in the behavior of sea level to analyze. The first system for reading the sea level was a tide board attached at the pier. In Spain the first modern tide gauge was installed in the Port of Alicante Mediterranean Sea in 1873 depending of the National Geographic Institute IGN. Just the following year a similar tide gauge was installed at the entrance of the Santander Bay. La Magdalena tide gauge was working during two periods 18761928 and 19631975. Together with Cdiz the IGN tide gauges were used to determinate the national datum for terrestrial cartography. The Spanish Institute of Oceanography IEO tide gauge network was initiated in 1943 with the installation of tide gauges along the Spanish coast. One of them was located in Santander and has been working since then. At the beginning it was a float tide gauge connected to a graphical continuous recorder. Nowadays it also has a digital encoder and a remote connection that allow using the recorded data for operational purposes. Later a Radar system was added. This tide gauge is referred to the Tide Gauge Zero and also calibrated to a benchmark in order to have a unique reference. This high quality sea level information is required for international and regional research activities as Global Sea Level Observing System GLOSS. In particular long time series are widely used for climate change detection. The sea level long term variability studies require a very good quality data focus in the reference of the data along the whole period and also it will be more precisely if we can remove the crustal movements by monitoring the tide gauge benchmark. Increase in sea level detected in the Santander tide gauge is more than 2 mmyear. Annual and semiannual cycles are detected in the monthly mean sea level. The amplitude of the annual cycle is 30 mm. and the semiannual 21 mm. Due to the good correlation between the NAO index and the monthly mean sea level we can assume that an important part of these cycles corresponds to the meteorological influence. The historical original records on paper are also digitalized images in order to avoid loses by paper degrading facilitate the access to them and in the future keep a higher frequency record for systematic studies of extreme events.

2017-04-01T00:00:00Z

['2017EGUGA..1915045L']

More than 70 years of continuous sea level records on the Santander Bay.

['PUB_PDF']

2018cosp...42E3546S

AcousticGravity Waves AGW generated by tsunamis propagating in the open ocean perturb the ionosphere and generate Traveling Ionospheric Disturbances TID. Recent investigations show that continuous monitoring of tsunamigenic TIDs can be used as a tsunami early warning system provided such TIDs are properly characterized in order to differentiate it from the TIDs of other origins. The characteristics of tsunamigenic TIDs are primarily derived with a point source approximation and thus assuming the wavefronts of the tsunamis are circular. However in reality the wavefronts of the tsunamis generated by the submarine earthquakes mimic the shape of the rupturing faults. Hence such simple approximations while studying the tsunamis generated by rupture of the fault with a length of 12001300 km in the case of 26th December 2004 SumatraAndaman tsunami and 500 km in the case of 11th March 2011 Tohoku tsunami will severely undermine the characteristics of the resultant TIDs. In this work we present characteristics of TIDs induced by the 26th December 2004 SumatraAndaman tsunami for the first time by considering the elliptical wavefront mimicking the entire fault geometry. Our results show that the magnitude of horizontal velocities of TIDs increase from 3.5 to 65 with respect to the direction of propagation of the tsunami when the actual geometry is considered in place of simple point source assumption. This establishes the significance of considering the actual fault geometry while deriving the TID characteristics. Further the results of crosswavelet analysis carried out between numerically simulated realistic tsunami wavefront and associated TIDs derived using GPS observations which reveal the dynamic coupling of tsunami and ionosphere are also discussed.

2018-07-01T00:00:00Z

['2018cosp...42E3546S']

Influence of source geometry in determining the characteristics of tsunamiinduced TIDs

2017CoBAO..64..116H

In 2014 a new monitoring project started at the observational base Saravand of the Byurakan astrophysical observatory. This project initiated for revealing natural and artificial objects at the nearEarth space. This is a kind of continuation of earlier observational projects implemented at the observatory prior the collapse of Soviet Union. This time nearEarth space monitoring is carried out at the request of the Russian agency ROSKOSMOS. For observations the EOP1 module is used which includes small telescopes with a mirror diameter of 40cm 25cm and 19cm.

2017-12-01T00:00:00Z

['10.52526/25792776-2017.1-116', '2017CoBAO..64..116H']

['Near-Earth space', 'artificial satellites', 'cosmic junk', 'monitoring']

New observational project for revealing natural and anthropogenic threats at the nearEarth space

['PUB_HTML', 'PUB_PDF']

2017CoBAO..64..102M

We present the Byurakan Astrophysical Observatory BAO Plate Archive Project that is aimed at digitization extraction and analysis of archival data and building an electronic database and interactive sky map. BAO Plate Archive consists of 37500 photographic plates and films obtained with 2.6m telescope 1m and 0.5m Schmidt telescopes and other smaller ones during 19471991. The famous Markarian Survey or the First Byurakan Survey FBS 2000 plates were digitized in 20022005 and the Digitized FBS DFBS www.aras.amDfbsdfbs.html was created. New science projects have been conducted based on this lowdispersion spectroscopic material. Several other smaller digitization projects have been carried out as well such as part of Second Byurakan Survey SBS plates photographic chain plates in Coma where the blazar ON 231 is located and 2.6m film spectra of FBS Blue Stellar Objects. However most of the plates and films are not digitized. In 2015 we have started a project on the whole BAO Plate Archive digitization creation of electronic database and its scientific usage. Armenian Virtual Observatory ArVO www.aras.amArvoarvo.htm database will accommodate all new data. The project runs in collaboration with the Armenian Institute of Informatics and Automation Problems IIAP and will continues during 4 years in 20152018. The final result will be an Electronic Database and online Interactive Sky map to be used for further research projects. ArVO will provide all standards and tools for efficient usage of the scientific output and its integration in international databases.

2017-12-01T00:00:00Z

['10.52526/25792776-2017.1-102', '2017CoBAO..64..102M']

['photographic plates', 'plate archives', 'digitization', 'astrometry', 'photometry', 'spectroscopy', 'databases', 'virtual observatories']

BAO Plate Archive Project

['PUB_HTML', 'PUB_PDF']

2017EGUGA..1916905B

Source Apportionment SA is the identification of ambient air pollution sources and the quantification of their contribution to pollution levels. This task can be accomplished using different approaches chemical transport models and receptor models. Receptor models are derived from measurements and therefore are considered as a reference for primary sources urban background levels. Chemical transport model have better estimation of the secondary pollutants inorganic and are capable to provide gridded results with high time resolution. Assessing the performance of SA model results is essential to guarantee reliable information on source contributions to be used for the reporting to the Commission and in the development of pollution abatement strategies. This is the first intercomparison ever designed to test both receptor oriented models or receptor models and chemical transport models or source oriented models using a comprehensive method based on model quality indicators and preestablished criteria. The target pollutant of this exercise organised in the frame of FAIRMODE WG 3 is PM10. Both receptor models and chemical transport models present good performances when evaluated against their respective references. Both types of models demonstrate quite satisfactory capabilities to estimate the yearly source contributions while the estimation of the source contributions at the daily level time series is more critical. Chemical transport models showed a tendency to underestimate the contribution of some single sources when compared to receptor models. For receptor models the most critical source category is industry. This is probably due to the variety of single sources with different characteristics that belong to this category. Dust is the most problematic source for Chemical Transport Models likely due to the poor information about this kind of source in the emission inventories particularly concerning road dust resuspension and consequently the little detail about the chemical components of this source used in the models. The sensitivity tests show that chemical transport models show better performances when displaying a detailed set of sources 14 than when using a simplified one only 8. It was also observed that an enhanced vertical profiling can improve the estimation of specific sources such as industry under complex meteorological conditions and that an insufficient spatial resolution in urban areas can impact on the capabilities of models to estimate the contribution of diffuse primary sources e.g. traffic. Both families of models identify traffic and biomass burning as the first and second most contributing categories respectively to elemental carbon. The results of this study demonstrate that the source apportionment assessment methodology developed by the JRC is applicable to any kind of SA model. The same methodology is implemented in the online DeltaSA tool to support source apportionment model evaluation httpsourceapportionment.jrc.ec.europa.eu.

2017-04-01T00:00:00Z

['2017EGUGA..1916905B']

Preliminary Results of the first European Source Apportionment intercomparison for Receptor and Chemical Transport Models

['PUB_PDF']

2013M&PSA..76.5342M

Cluster chondrite clasts with distinct chondrule populations occur in the same UOC breccia. This indicates repeated chondrule forming events or the creation of different chondrule populations during a single event by sizesorting.

2013-09-01T00:00:00Z

['2013M&PSA..76.5342M']

Distinct Chondrule Populations in Different UOC Cluster Chondrite Clasts

['PUB_PDF']

2017Ciel...79..546M

Gographie de Pluton Qui nous observe Pulsar binaire record Rayons cosmiques nergtiques Ondes gravitationnelles U Antliae 40 Eridani BC Lastrode 2006 VW139288P Fron cosmique Tempte de neige sur Mars Oxyde de titane sur Wasp19b La matire organique des comtes Chondrites carbones

2017-11-01T00:00:00Z

['2017Ciel...79..546M']

Lastronomie dans le monde

2017Ciel...79..542N

Cadran situ rue du Vlodrome 102 Retinne

2017-11-01T00:00:00Z

['2017Ciel...79..542N']

Cadrans solaires de Wallonie

2018cosp...42E3160S

Nonthermal particle distributions are ubiquitous in the solarwind and near Earth space plasma their presence having frequently been confirmed by interplanetary missions. Such distributions represent suprathermal deviations from the Maxwellian equilibrium and are expected to exist in any lowdensity plasma in the Universe where binary collisions of charges are sufficiently rare. The suprathermal populations are well parameterized by the socalled Kappa index. Moreover inhomogeneity may arise in plasma from the equilibrium dust density gradient. Even if the dust density is kept uniform the plasma density gradient can still significantly affect dust acoustic solitary waves DASWs through the equilibrium dust charge because the dust grain charge is selfconsistently determined by plasma charging currents that depend on plasma densities. In this case the equilibrium dust charge instead of density becomes spatially nonuniform. In such a case inhomogeneity is generated by electron and ion density gradients in the plasma and the amplitude of DASWs is mainly affected by density inhomogeneity rather than the electrons energy. We investigate dust acoustic nonlinear structures in unmagnetized inhomogeneous dusty plasma containing superthermal electrons and ions. In this model the electrons and ions are described by the kappa distribution function and dustneutral collisions have been taken into account. Using the reductive perturbation method Modified Burgers equation will be derived. Our study would be useful for understanding different nonlinear features of localized electrostatic disturbances in a number of astrophysical dusty plasma systems namely planetary rings cometary environments and the interstellar medium where density inhomogeneity of charged particles is prevalent.

2018-07-01T00:00:00Z

['2018cosp...42E3160S']

Effect of density gradient on nonlinear structures in a dusty plasma

2014yCat..22100001C

During the first 10 months of science operations more than 2000 solartype stars were selected by the Kepler Asteroseismic Science Consortium KASC to be observed as part of an asteroseismic survey of the Sunlike population in the Kepler field of view. Solarlike oscillations were detected by Kepler in more than 500 stars Chaplin et al. 2011Sci...332..213C and from these data robust global or average asteroseismic parameters were determined for all targets in the sample. These asteroseismic parameters allow us to estimate fundamental properties of the stars. In this paper we present stellar properties namely masses radii surface gravities mean densities and ages of this asteroseismic sample of mainsequence and subgiant stars. P 5 data files.

2014-01-01T00:00:00Z

['2014yCat..22100001C', '10.26093/cds/vizier.22100001']

['Abundances: [Fe/H]', 'Effective temperatures', 'Stars: masses', 'Stars: ages']

VizieR Online Data Catalog Asteroseismic study of solartype stars Chaplin 2014

['PUB_HTML']

2017AdSpR..59.2407M

Uranus together with Neptune in our Solar System belongs to a class of planets called ice giants which have never been explored using a dedicated mission. A mission to explore the ice giants is one of the highest priority missions of NASA. In this paper we present a new and unique multiprobe multiplanet spacecraft to explore two of the outer planets Saturn and Uranus. The mission concept addresses the highpriority science goals of Saturn and Uranus as set forth by the National Research Councils Planetary Sciences Decadal Survey Visions and Voyages for Planetary Science in the Decade 20132022. The growing importance of understanding the evolution and role of ice giants in extrasolar planetary systems makes Uranus a pertinent scientific target. The mission concept employs the Space Launch System to deliver a 1700 kg orbiter to Uranus using a ballistic SaturnUranus trajectory with a timeofflight of 11.5 years. The baseline mission concept includes two atmospheric entry probes one deployed at Saturn and another at Uranus prior to an impulsive orbit capture. A payload of nine remote sensing and in situ plasma instruments onboard the orbiter support a broad array of investigations during the nominal 2year science mission. P In addition to the baseline concept system trade studies were conducted to explore the advantages of aerocapture and use of the Space Launch System. Based on the results of these trade studies a preferred point design within constraints of NASAs Flagship program can be launched in the late 2020s. A neural network model using analogybased data was developed to estimate the mission cost which was found to be 1.9 billion in FY15.

2017-05-01T00:00:00Z

['10.1016/j.asr.2017.02.012', '2017AdSpR..59.2407M']

['Ice giants', 'Mission design', 'Outer planets', 'Saturn', 'Uranus']

Oceanus A multispacecraft flagship mission concept to explore Saturn and Uranus

['PUB_HTML']

2014AGUFMSH21C4129P

Extreme Space Weather events are large solar flares or geomagnetic storms which can cost billions of dollars to recover from. We have few examples of such events the Carrington Event the solar superstorm is one of the few that had superlatives in three categories size of solar flare drop in Dst and amplitude of aa. Kepler observations show that stars similar to the Sun can have flares releasing millions of times more energy than an Xclass flare. These flares and the accompanying coronal mass ejections could strongly affect the atmosphere surrounding a planet. What level of solar activity would be necessary to strongly affect the atmosphere of the Earth Can we map out the envelope of space weather along the evolution of the Sun What would space weather look like if the Sun stopped producing a magnetic field To what extreme should Space Weather go These are the extremes of Space Weather explored in this talk.

2014-12-01T00:00:00Z

['2014AGUFMSH21C4129P']

['7524 Magnetic fields', 'SOLAR PHYSICS', 'ASTROPHYSICS', 'AND ASTRONOMY', '7536 Solar activity cycle', 'SOLAR PHYSICS', 'ASTROPHYSICS', 'AND ASTRONOMY', '7594 Instruments and techniques', 'SOLAR PHYSICS', 'ASTROPHYSICS', 'AND ASTRONOMY', '7938 Impacts on humans', 'SPACE WEATHER']

Pushing the Envelope of Extreme Space Weather

2023yCat..19210122M

Both rho CrB and 88 Leo have synoptic Sindex time series from the Mount Wilson Observatory MWO HK Project ranging from near the beginning of the program in 1966 to its termination in 2003 see Figure 1. The MWO Sindex measures the ratio of emission from 1 cores of the CaII H and K lines to the sum of two nearby 20 pseudocontinuum bandpasses. See Section 2.1. P The Transiting Exoplanet Survey Satellite TESS observed rho CrB in 2minute cadence for a total of approximately 52 days during Sectors 24 and 25 of Cycle 2 2020 April 152020 June 08. TESS observed 88 Leo in 2minute cadence for a total of approximately 27 days during Sector 22 of Cycle 2 2020 February 182020 March 18. See Section 2.2. P We obtained a Chandra observation of rho CrB using the High Resolution Camera imaging detector HRCI on 2020 April 19 starting at UT 1459 for a net exposure time of 11870s ObsID 22308. An earlier observation of rho CrB had also been obtained PI S. Saar several years earlier on 2012 January 17 beginning at UT 1312 using the Advanced CCD Imaging Spectrometer spectroscopic array ACISS on the backilluminated CCD s3 for a net exposure of 9835s obsID 12396. See Section 2.4. P 2 data files.

2023-02-01T00:00:00Z

['10.26093/cds/vizier.19210122', '2023yCat..19210122M']

['Asteroseismology', 'Stars: G-type', 'Stars: diameters', 'Stars: masses', 'Stars: ages', 'Optical', 'X-ray sources']

VizieR Online Data Catalog Chromospheric activity of rho CrB and 88 Leo Metcalfe 2021

['PUB_HTML']

2018cosp...42E3277S

Millimetron observatory under development at the Lebedev Physical Institute includes a spacebased 10meter telescope operating at millimeter and infrared wavelengths from 0.02 to 17 mm millimetron.ru. In the singledish mode it can detect exoplanets in the lowest spectral band. We provide the list of exoplanets that would be available to Millimetron according to its planned sensitivity. We take into account different sources of the candidates radiation reradiation of the energy of the host star and the proper flux contribution of which is important for young and hot exoplanets. Also we consider transits and the respective decrease in flux.

2018-07-01T00:00:00Z

['2018cosp...42E3277S']

Exoplanetary candidates to observations with Millimetron

2014yCat..35720034G

We used data collected by the NASA planethunter mission Kepler. P 2 data files.

2014-10-01T00:00:00Z

['10.26093/cds/vizier.35720034', '2014yCat..35720034G', '2014yCat..35729034G']

['Stars: G-type', 'Stars: variable']

VizieR Online Data Catalog Pulsating solarlike stars in Kepler Garcia 2014

['PUB_HTML']

2018cosp...42E3823Z

Double neutron star DNS merger events are promising candidates of short Gammaray Burst sGRB progenitors as well as highfrequecy gravitational wave GW emitters. On August 17 2017 such a coinciding event was detected by both the LIGOVirgo gravitational wave detector network as GW170817 and GammaRay Monitor on board NASAs Fermi Space Telescope as GRB 170817A. Here we show that the fluence and spectral peak energy of this sGRB fall into the lower portion of the distributions of known sGRBs. Its peak isotropic luminosity is abnormally low. The estimated event rate density above this luminosity is at least 190 per cubic Gpc per yr which is close to but still below the DNS merger event rate density. This event likely originates from a structured jet viewed from a large viewing angle. There are similar faint soft GRBs in the Fermi archival data a small fraction of which might belong to this new population of nearby lowluminosity sGRBs.

2018-07-01T00:00:00Z

['2018cosp...42E3823Z']

A peculiar lowluminosity short gammaray burst from a double neutron star merger progenitor

2017CBET.4367....3W

The available astrometry spanning Feb. 1028 the following preliminary parabolic orbital elements by G. V. Williams and an ephemeris appear on MPEC 2017E06. T 2017 Apr. 29.5264 TT Peri. 341.1099 Node 186.5945 2000.0 q 4.967364 AU Incl. 125.6559

2017-03-01T00:00:00Z

['2017CBET.4367....3W']

Comet C2017 D3 Atlas

['PUB_HTML']

2017EGUGA..1916366H

The Ganymede Laser Altimeter GALA is one of the instruments selected for ESAs Jupiter Icy Moons Explorer JUICE. A fundamental goal of any exploratory space mission is to characterize and measure the shape topography and rotation of the target bodies. A state of the art tool for this task is laser altimetry because it can provide absolute topographic height and position with respect to a body centered reference system. With respect to Ganymede the GALA instrument aims at mapping of global regional and local topography confirming the global subsurface ocean and further characterization of the watericeliquid shell by monitoring the dynamic response of the ice shell to tidal forces providing constraints on the forced physical librations and spinaxis obliquity determining Ganymedes shape obtaining detailed topographic profiles across the linear features of grooved terrain impact structures possible cryovolcanic features and other different surface units providing information about slope roughness and albedo at 1064nm of Ganymedes surface. After several flybys Ganymede Europa Callisto it is scheduled that the JUICE orbiter will enter first into an elliptical orbit 200 km x 10.000 km for around 150 days and then into a circular orbit 500 km around Ganymede for 130 days. Accordingly to the different orbits and trajectories distances to the moons respectively the spot size of the GALA laser varies between 21 m and 140 m. GALA uses the directdetection classical approach of laser altimetry. Laser pulses are emitted at a wavelength of 1064 nm by using an actively Qswitched NdYag laser. The pulse energy and pulse repetition frequency are 17 mJ at 30 Hz nominal respectively. For targeted observations and flybys the frequency can be switched to 50 Hz. The emission time of each pulse is measured by the detector. The beam is reflected from the surface and received at a 25 cm diameter telescope. The returning laser pulse is refocused onto a silicon avalanche photodiode APD through backend optics including a narrow bandpass interference filter for isolating the 1064 nm wavelength. The APDsignal is then amplified sampled and fed to a digital range finder. This system determines the time of flight pulse intensity width and full shape. The GALA instrument is developed in collaboration of institutes and industry from Germany Japan Switzerland and Spain.

2017-04-01T00:00:00Z

['2017EGUGA..1916366H']

Status of the Ganymede Laser Altimeter GALA for ESAs Jupiter Icy Moons Explorer JUICE

['PUB_PDF']

2017EGUGA..1915803N

The central European lake district extends within the Bohemian forest and Bavarian forest Mountains. It includes 8 glacial lakes extending in altitudes from 935 to 1087 m a.s.l. All of them have been oligotrophic and forests of the lake catchments are dominated by Norway spruce Picea abies. Plen lake PL catchment is at 1087 m .a.s.l. and it covers area of 0.67 km2. In 2004 the forest at PL catchment was infested by the bark beetle Ips typographus and 8899 of trees had died by 2011. In contrast to relatively detailed research of North American and Scandinavian lake ecosystems the information concerning Hg contamination of central European lake ecosystems are rather scarce. The PL ecosystem can provide base for assessment of Hg contamination as well as for changes induced by the bark beetle infestation. In 2016 mean annual Hg concentration in bulk precipitation at Plen lake reached 3.0 ngL and bulk Hg deposition flux amounted at 4.6 gm2. The most important pathway of Hg deposition to the forest ecosystems has been litterfall. The highest Hg concentrations in litterfall material at PL were found in lichens 205 gkg mixture of unidentifiable organic debris 159 gkg and bark 123 gkg. Litterfall spruce needles averaged at 56 gkg only. Removal of spruce due to bark beetle infestation caused decrease of litterfall Hg fluxes. Recent litterfall fluxes in the unimpacted stands reached 55.8 gm2 while in the impacted dead stands they amounted 23.0 gm2 only. The qualitative composition of the litterfall in the infested stands was typical with absence of needles and prevalence of twigs and bark. To assess changes in Hg distribution within the soil profile due to forest dieback the soil data from year 1999 were compared with 2015 data. The mean Hg concentrations in the O horizons decreased from 424 to 311 gkg between years 1999 and 2015 and in A horizons the situation was reversed and an increase from 353 to 501 gkg occurred. The means of Hg concentration in mineral soil remained relatively similar at 145 and 121 gkg. Increased Hg concentrations in A horizons were concurrent with increased organic C concentrations from 24.5 in 1999 to 39.9 in 2015. Ratio HgC in the A horizon remained rather comparable 1.27 and 1.47. In O horizons HgC ratio decreased from 0.9 to 0.5 comparing 1999 and 2015 due to changes in litterfall composition and total deposition due to canopy absence since 2005. Tributaries and lake water Hg concentrations were assessed to estimate the fluxes of Hg within lake catchment. PL lake water contained on average 4.4 ngL of Hg and 8.2 mgL of DOC. Mean annual Hg concentration in four lake tributaries ranged from 2.0 to 16.5 ngL. The differences in Hg concentrations among individual streams were driven by DOC concentrations ranging from 2.1 to 21.2 mgL. The differences between the Hg and DOC concentrations tributaries result from differences in hydrology of the individual subcatchments. The financial support was provided by the Czech Science Foundation project No. GA1614762S.

2017-04-01T00:00:00Z

['2017EGUGA..1915803N']

Mercury in the central European lake district case study Plen lake

['PUB_PDF']

2017Ge&Ae..57..190P

The 22year variation in the frequency of aurora occurrence is found through an analysis of data of the Russian network of meteorological stations from 18371909. This variation is obtained in a form of asymmetry between even and odd solar cycles. We found that the nature of the 22year variation depends on the latitude of the observation station. The annual number N of midlatitude auroras geomagnetic latitudes lt 56 for about three years at the end of the descending part of solar cycles is larger for the even cycles than for the odd. For highlatitude auroras 56 the pattern is opposite at the descending part of the solar cycle N is larger in the odd cycles than in the even. For the highlatitude sector asymmetry of the polar sun cycles the period between two magnetic field reversals is clearly observed an increased N is observed during the whole odd polar cycle which starts approximately at the maximum of the odd Schwabe cycle as compared to the even cycle. Extrapolation of the modern picture of alternation of the sign of the global solar magnetic field back in time leads to the conclusion that the most geoeffective polar cycles in cycles 814 were those in which the polar magnetic field in the northen hemisphere was negative.

2017-03-01T00:00:00Z

['10.1134/S0016793217020116', '2017Ge&Ae..57..190P']

22year cycle in the frequency of aurora occurrence in XIX century Latitudinal effects

['PUB_HTML']

2024SPIE13096E..28K

GHOST is a newly operational optical fiberfed highresolution spectrograph at the Gemini South 8.1m telescope. It currently offers the choice of two resolution modes captured by one or two input IFUs with a FOV of 1.2 and a spectral resolving power of 56000 and 76000 for the unbinned CCDs. At the highresolution mode one can also instigate a simultaneous ThXe calibration lamp which along with a simultaneous pseudoslit profile constructed from reformatting the input IFU image will allow for precision radial velocity measurements. Here we talk about the proposed roadmap towards full queue operations potential upgrades and the error terms contributing to the final onsky RV precision which is estimated to be in the 110msSUP1SUP range.

2024-07-01T00:00:00Z

['2024SPIE13096E..28K', '10.1117/12.3021130']

Roadmap of GHOSTGeminis precision radial velocity mode

['PUB_HTML']

2013ICRC...33.3447B

TeV gammaray emission has been recently observed from the direction of open clusters containing many massive stars and dense concentrations of matter. We consider the high energy processes occurring within the massive binary systems and also within their environment by assuming that nuclei from the stellar winds are accelerated within the binary systems. We calculate the rates of injection of protons and neutrons from fragmentation of these nuclei in dense radiation field of the massive companion in binary system. Protons and neutrons from fragmentation of nuclei and nuclei itself interact with the matter of the stellar wind and that surrounding the binary system producing pions which decay into yrays and neutrinos. We discuss the detectability of such yray emission from the open clusters by the present and future Cherenkov telescopes. We also estimate the accompanying neutrino fluxes which are confronted with the sensitivity of IceCube.

2013-01-01T00:00:00Z

['2013ICRC...33.3447B']

['binaries: general — radiation mechanisms: non-thermal — gamma-rays: theory']

Gammarays and Neutrinos Produced Around Massive Binary Systems by Nuclei Accelerated Within the Binaries

['ADS_PDF', 'ADS_SCAN']

2017IJMPA..3250148W

The 21dimensional KleinGordon oscillator under a magnetic field in the presence of a minimal length in the noncommutative NC space is analyzed via the momentum space representation. Energy eigenvalue of the system is obtained by employing the Jacobi polynomials. In further steps the special cases are discussed and the corresponding numerical results are depicted respectively.

2017-09-01T00:00:00Z

['2017IJMPA..3250148W', '10.1142/S0217751X17501482']

['Klein–Gordon oscillator', 'noncommutative space', 'minimal length', '03.65.Pm', '04.20.Jb', 'Relativistic wave equations', 'Exact solutions']

21dimensional KleinGordon oscillator under a magnetic field in the presence of a minimal length in the noncommutative space

['PUB_HTML', 'PUB_PDF']

2024SPIE13102E..26M

Atmospheric interference noise and attenuation are a few limitations that arise when observing emissions of submillimeter wavelengths using groundbased telescopes. Ongoing research conducted on highaltitude balloons allow a new direction in observing these distributed emissions and eliminates all possible atmospheric interference. All submillimeter balloons and groundbased telescopes could benefit from a compact reconfigurable high gain programmable amplifier module to use in their receivers. We have designed built and tested an amplifier module for the Astrophysics Stratospheric Telescope for High Spectral Resolution Observations at Submillimeter wavelengths ASTHROS which is a highaltitude balloon mission that utilizes highspectral resolution spectrometry to analyze stellar feedback by mapping ionized gas from the Milky Way galaxy and other neighboring galaxies. Using a fivestage Intermediate Frequency IF Low Noise Amplifier LNA added to a readout chain using commercial offtheshelf components the amplifier module yields 74 dB of gain up to 3.5 GHz with 31.75 dB of programmable attenuation with relatively linear gain flatness of 1 dB all while consuming 2.25 W per module 9 V at 250 mA. BRBR BRBR While the amplification techniques and technology in this field are not new achieving such high gain in systems usually require a significant amount of space to be allocated onboard. To alleviate this issue this amplifier module has a unique form factor that combines the entire amplifier chain and bias system all in one module saving space and weight on the system. The form factor design also allows the module to be stacked on top of one another to provide a higher range of gain in the system. Currently the modules can be stacked up to eight times and can be connected to allow for full control of the system with the use of a microcontroller. Submillimeter systems can have a set of 8 modules all while saving space and reducing used weight.

2024-08-01T00:00:00Z

['10.1117/12.3018025', '2024SPIE13102E..26M']

A customizable fivestage intermediate frequency lownoise amplifier and readout chain for the Astrophysics Stratospheric Telescope for Highspectral Resolution Observations at Submillimeterwavelengths ASTHROS

['PUB_HTML']

2024SPIE13097E..0VT

With the commissioning of the refurbished adaptive secondary mirror ASM for the 6.5meter MMT Observatory under way special consideration had to be made to properly calibrate the mirror response functions to generate an interaction matrix IM. The commissioning of the ASM is part of the MMT Adaptive optics exo Planet characterization System MAPS upgrade the observatorys legacy adaptive optics AO system. Unlike most AO systems MAPS employs a convex ASM which prevents the introduction of a calibration source capable of simultaneously illuminating its ASM and wavefront sensor WFS. This makes calibration of the AO system a significant hurdle in commissioning. To address this we have employed a hybrid calibration strategy we call the Efficient Synthesis of Calibrations for Adaptive Optics through Pseudosynthetic and Empirical methods ESCAPE. ESCAPE combines the DOCRIME onsky calibration method with the SPRINT method for computing pseudosynthetic calibration matrices. To monitor quasistatic system change the ESCAPE methodology rapidly and continuously generates pseudosynthetic calibration matrices using continual empirical feedback in either open or closedloop. In addition by measuring the current IM in the background while in closeloop we are also able to measure the optical gains for pyramid wavefront sensor PyWFS systems. In this paper we will provide the mathematical foundation of the ESCAPE calibration strategy and onsky results from its application in calibrating the MMT Observatorys ASM. Additionally we will showcase the validation of our approach from our AO testbed and share preliminary onsky results from MMT.

2024-08-01T00:00:00Z

['10.1117/12.3020489', '2024SPIE13097E..0VT']

ESCAPE efficient synthesis of calibrations for adaptive optics through pseudosynthetic and empirical methods

['PUB_HTML']

2017EGUGA..1915532J

The monthly global gravity field solutions derived using the measurements from the GRACE Gravity Recovery and Climate Experiment satellites have been continuously improved by the processing centers. One of the improvements in the processing method is a more detailed calibration of the onboard accelerometers in the GRACE satellites. The accelerometer data calibration is usually restricted to the scale factors and biases. It has been assumed that the three different axes are perfectly orthogonal in the GRACE science reference frame. Recently it was shown by Klinger and MayerGrr 2016 that a fullypopulated scale matrix considering the nonorthogonality of the axes and the misalignment of the GRACE science reference frame and the GRACE accelerometer frame improves the quality of the C20 coefficient in the GRACE monthly gravity field solutions. We investigate the effect of the more detailed calibration of the GRACE accelerometer data on the C20 coefficient in the case of the AIUB Astronomical Institute of the University of Bern processing method using the Celestial Mechanics Approach. We also investigate the effect of the new calibration parameters on the stochastic parameters in the Celestial Mechanics Approach.

2017-04-01T00:00:00Z

['2017EGUGA..1915532J']

Effect of the improved accelerometer calibration method on AIUBs GRACE monthly gravity field solution

['PUB_PDF']

2017EGUGA..1915411K

Installed onboard the German research aircraft HALO the integratedpath differentialabsorption IPDA lidar CHARMF measures weighted vertical columns of the greenhouse gases CO2 and CH4 below the aircraft and along its flight track aiming at high accuracy and precision. CHARMF was designed and built as an airborne demonstrator for the space lidar MERLIN the Methane Remote Lidar Mission conducted by the German and French space agencies DLR and CNES with launch foreseen in 2021. It provides excellent opportunities for targeted measurements of regional fluxes and hot spots. We present exemplary measurements from several flights performed in spring 2015 over Central Europe. Our analyses reveal a measurement precision of below 0.5 for 20km averages. A methane plume from a coal mine ventilation shaft was overflown as well as a carbon dioxide plume from a large coalfired power plant. The method to estimate fluxes from the lidar signals will be explained. The results show good agreement with reported emission rates. The airborne measurements are expected to improve the retrieval of future spaceborne IPDA lidar systems such as MERLIN. CHARMF measurements over mountains water and clouds help assess the strength and variability of backscatter from such challenging surfaces. The IPDA weighting function or measurement sensitivity is dependent on atmospheric pressure and temperature. We use ECMWF analyses interpolated in space and time to the aircraft track that provide these auxiliary data. The relatively coarse model representation of orography with respect to the lidar causes uncertainties that we assess. CHARMF will be a key instrument in the upcoming CoMet field experiment where active and passive remote sensing as well as insitu instruments will be installed onboard HALO. The flights are scheduled in April and May 2017 over Central Europe and will focus on point sources such as power plants coal mines and landfills as well as on urban gradients and more extended sources such as agriculture and wetlands.

2017-04-01T00:00:00Z

['2017EGUGA..1915411K']

Test Flight Results of the New Airborne CH4 and CO2 Lidar CHARMF

['PUB_PDF']

2017EGUGA..1915513D

Little is known about compositional and structural diversity of super Earths. SuperEarths are distinct from miniNeptunes in terms of the origin of their atmospheres i.e. which are outgassed from the interior. Modeling the outgassing rates that arise from interior dynamics is key in order to inform the interpretation of data from current and future missions e.g. James Webb Space telescope. Here we present a comprehensive study on the outgassing of superEarths of different mass structure composition and temperature. We emphasize that this study is limited to planets in a stagnantlid convection regime only. We model a convection and melting in a 2D spherical annulus geometry. The convection code solves the conservation equations for mass momentum and energy. Partial melt occurs where mantle temperature exceeds the solidus melting temperature. If the melt is gravitationally buoyant we assume that melt rises immediately to the surface while tracing the melt depletion in the mantle with particles that advect along the convective stream lines. The model for convection and melting is applied to planets between 1 and 8 Earth masses. Besides planet mass we test different aspects that may influence the production of melt and outgassing 1 core size 2 mantle composition especially iron mantle content 3 upper mantle temperature 4 amount of radioactive heat sources 5 temperature jump at the coremantleboundary 6 lithosphere thickness and 7 model resolution. We present our findings in the form of scaling laws that express the outgassing depending on investigated parameters. We find that first order effects on outgassing are energyrelated parameters such as upper mantle temperature and the amount of radioactive heat sources as well as planet mass. Interestingly the composition of the mantle has only secondorder effects. However we note that we use reference profiles for pressure and temperature and hence phase transition depths are set constant over time. Core size has almost no effect on melting in the mantle. Findings of our study are in agreement with previous work. Our study however represents a comprehensive investigation of interior parameters that affect melting and outgassing. We provide scaling laws of outgassing that are helpful for the interpretation of astrophysical data from superEarths atmospheres.

2017-04-01T00:00:00Z

['2017EGUGA..1915513D']

Outgassing of stagnantlid planets

['PUB_PDF']

2024PhRvC.109b5803R

We have previously shown R. Rizaldy A. R. Alfarasyi A. Sulaksono and T. Sumaryada Phys. Rev. C 100 055804 2019 10.1103PhysRevC.100.055804 that Fermisurface distortion can affect nuclear matter and neutron star NS properties within the relativistic meanfield formalism. However our previous results had the caveat that the kSUBfSUBMSUPSUPlt1 approximation was used. This approximation needs revision for highdensity NS cases. This work proposes a more refined approximation in calculating the Fermisurface distortion correction. We reinvestigate the consequences in nuclear and NS matter. The new expressions of the corresponding nucleon densities energy density and pressures are shown. The behavior of the predictions in highdensity regions is studied. We found a better convergence of results for higher values than in the previous work. We also found that all recent experimental observations and other calculations constrain the acceptable value of to 0.1 . We also study the impact of Fermisurface distortion on NS mass radius moment of inertia and tidal deformability. The results are compared to the recent observation data. The impact of the anisotropy of acceptable values still does not profoundly impact a NSs mass and moment of inertia. However we also observed a substantial effect in tidal deformation properties such as and kSUB2SUB parameters. Therefore the signature of Fermisurface distortion might be detected in observations of gravitational waves.

2024-02-01T00:00:00Z

['10.1103/PhysRevC.109.025803', '2024PhRvC.109b5803R']

Impact of Fermisurface distortion in a relativistic meanfield model on the moment of inertia and tidal deformability of neutron stars

['PUB_HTML']

2017EGUGA..1916160H

Soil moisture is one of the terrestrial essential climate variables that has critical role in the water energy and carbon cycles. There are different ways available for the retrieval of this essential variable e.g. remote sensing hydrological models insitu measurements and etc.. However the time series of these retrievals often contain systematic differences which need to be removed via different rescaling approaches before these data sets could be used in data fusion type studies. In this study the added utility of nonlinear rescaling methods relative to linear methods in the framework of data fusion has been explored. Nonlinear rescaling methods implemented in this study include multivariate adaptive regression splines MARS Support vector machines SVM and artificial neural network ANN while the linear methods include linear regression variancematching and triple collocation. Land Parameter Retrieval Model LPRM and NOAH soil moisture datasets are rescaled into the space of insitu measurements obtained over four United States Department of Agriculture USDA Agricultural Research Service ARS watersheds and later merged using a simple linear weighting method. Validation of the fused products using linear and nonlinear methods show that on average fusing of nonlinearly rescaled LPRM and NOAH soil moisture products yields 3 percent correlation i.e. against the in situ data improvement against nonlinearly rescaled NOAH soil moisture product while this improvement is more than 5 percent when the fused product is compared against the linearly rescaled NOAH product.

2017-04-01T00:00:00Z

['2017EGUGA..1916160H']

Investigation of the impact of the nonlinear relations among soil moisture products over data fusion process

['PUB_PDF']

2017EGUGA..1917148O

Spectral images of Mars recorded by OMEGA Observatoire pour la Minralogie lEau les Glaces et lActivit on Mars Express can be used to deduce the mean effective radius reff and optical depth i of water ice particles in clouds. Using new data sets for a priori surface temperature vertical profiles of atmospheric temperature dust opacity and multispectral surface albedo we have analyzed over 40 OMEGA image cubes over the Tharsis Arabia and Syrtis Major quadrangles and mapped the spatial distribution of reff i and water ice column mass. We also explored the parameter space of reff and i which are inversely proportional and the ice cloud index ICI which is the ratio of the reflectance at 3.4 and 3.52 m and indicates the thickness of water ice clouds. We found that the ICI trivial to calculate for OMEGA image cubes can be a proxy for column mass which is very expensive to compute requiring accurate retrievals of surface albedo reff and i. Observing the spatial distribution we find that within each cloud system reff varies about a mean of 2.1 m that SUBiSUB is closely related to reff and that the values allowed for i given reff are related to the ICI. We also observe areas where our retrieval detects very thin clouds made of very large particles mean of 12.5 m which are still under investigation.

2017-04-01T00:00:00Z

['2017EGUGA..1917148O']

Water ice cloud property retrievals at Mars with OMEGASpatial distribution and column mass

['PUB_PDF']

2017EGUGA..1915618J

Shock waves are ubiquitous in the universe and act to slow down and heat supersonic flows. In collisionless space plasmas shocks are able to accelerate particles to very high energy through various processes. Many processes relating to shock nonstationarity and plasma dynamics are subgyroscale and have therefore previously been difficult to study. The Magnetospheric MultiScale MMS mission provides a unique view of Earths bow shock. With the close spacecraft separation of 740km and highcadence particle and field measurement MMS enables studies of the dynamics of plasma and structure of the shock at small spatial and temporal scales. We present recent results from MMS relating to shock nonstationarity. In particular we discuss observations that reveal motion of the shock surface back and forth across the spacecraft due to ripples moving along the shock front. We compare different shockcrossings by MMS and test models of shock nonstationarity.

2017-04-01T00:00:00Z

['2017EGUGA..1915618J']

Shock nonstationarity observed by MMS

['PUB_PDF']

2017EGUGA..1916029A

The Max Planck Institute for Biogeochemistry MPIBGC has been operating a FourierTransform Spectrometer FTS on Ascension Island 8 S 14 W as part of the Total Carbon Column Observation Network TCCON. Since 2012 this instrument has been observing columnaveraged dryair mole fractions commonly referred to as Xgas of greenhouse gases like CO2 CH4 CO N2O and others. Due to its location in the southern trade wind zone the station is downwind from Africa most of the time. Different parts of the total column above the station are influenced by fluxes from different regions. Especially the lower layers of the free troposphere just above the planetary boundary layer PBL show strong biomass burning signals. XCH4 and especially XCO are strongly enhanced during the northern and southern African burning seasons. For XCO enhancements of 50100 in the total column can be observed on the time scale of days. Transport model simulations suggest that biomass burning signals from as far as the Eastern Indian Ocean may be detected over Ascension Island. Most of these effects are not visible from observations in the PBL. The 5year time series allows a first look at the effect of the 201516 El Nio on the biomass burning patterns in the Southern Hemisphere.

2017-04-01T00:00:00Z

['2017EGUGA..1916029A']

Biomass burning signals over the South Atlantic Ocean before and during the El Nio event of 201516

['PUB_PDF']

2017EGUGA..1914639Z

The FERMILAT gammaray experiment observed a surprisingly large number of solar events with gammaray emission above photon energies of 100 MeV. The emission is likely due to piondecay photons. This implies that the acceleration of protons in the solar corona to energies above 300 MeV is much more frequent than previously thought. In some cases the emission persists over several hours. In the frame of the HESPERIA project funded by the Horizon 2020 programme of the European Union we conduct an extensive study on the relationship between these gammaray emissions and electromagnetic signatures of accelerated electrons in the corona. This contribution is to present the results on a sample of 25 gammaray events some with a very long duration signature gt 6 hours and some with a shorter duration lt1 hour starting immediately after the impulsive phase. We compare the durations of the gammaray emission with the durations of hard Xray metric decametric and microwave signatures to see if longduration gammaray events are accompanied by signatures of longduration electron acceleration. In our sample we found the presence of type IV radio emission in the metric and decimetric range lasting several hours to be associated only with the gammaray events of very long duration. We also show that in each gammaray event electrons had rapid access to interplanetary space since the impulsive flare phase so that highenergy SEP events should be detected. Acknowledgements This project has received funding from the European Unions Horizon 2020 research and innovation program under grant agreement No 637324

2017-04-01T00:00:00Z

['2017EGUGA..1914639Z']

HESPERIA studies on the nature of highenergy solar gammaray events

['PUB_PDF']

2017EGUGA..1916489F

Motherofpearl clouds appear irregularly in the winter stratosphere at high northern latitudes about 2030 km above the surface of the Earth. The size range of the cloud particles is near that of visible light which explains their extraordinary beautiful colours. We argue that the Norwegian painter Edvard Munch could well have been terrified when the sky all of a sudden turned bloodish red after sunset when darkness was expected. Hence there is a high probability that it was an event of motherofpearl clouds which was the background for Munchs experience in nature and for his iconic Scream. Currently the leading hypothesis for explaining the dramatic colours of the sky in Munchs famous painting is that the artist was captivated by colourful sunsets following the enormous Krakatoa eruption in 1883. After carefully considering the historical accounts of some of Munchs contemporaries especially the physicist Carl Strmer we suggest an alternative hypothesis namely that Munch was inspired by spectacular occurrences of motherofpearl clouds. Such clouds which have a wavelike structure akin to that seen in the Scream were first observed and described only a few years before the first version of this motive was released in 1892. Unlike clouds related to conventional weather systems in the troposphere motherofpearl clouds appear in the stratosphere where significantly different physical conditions prevail. This result in droplet sizes within the range of visible light creating the spectacular colour patterns these clouds are famous for. Carl Strmer observed such clouds and described them in minute details at the age of 16 but already with a profound interest in science. He later noted that ..these motherofpearl clouds was a vision of indescribable beauty The authors find it logical that the same vision could appear scaring in the sensible mind of a young artist unknown to such phenomena.

2017-04-01T00:00:00Z

['2017EGUGA..1916489F']

Screaming Clouds

['PUB_PDF']

2017EGUGA..1917145J

The Mercury Orbiter Radioscience Experiment MORE is one of the instruments on board the BepiColombo Mercury Planetary Orbiter MPO designed to estimate the Mercurys gravity field and rotational state and to perform a wide set of tests of relativistic gravity. The experiments exploits a highly stable multifrequency radio links in X and Ka band. The stateoftheart microwave equipment enables simultaneous twoway links in XX 7.2 GHz uplink8.4 GHz downlink XKa 7.232.5 GHz and KaKa band 3432.5 GHz providing range rate accuracies of 3 microns at 1000 s integration time at nearly all elongation angles. Range observables accurate to 20 cm twoway will be attained using a novel wideband 24 Mcps ranging system based upon a pseudonoise modulation scheme. Nongravitational acceleration will be provided by a dedicated accelerometer the Italian Spring Accelerometer ISA. We present the results of numerical simulations carried out using the latest mission scenario entailing a launch date in October 2018 with arrival in Mercury in December 2025. We illustrate as the combination of the gravity and rotation measurements expected from BepiColombo can bring a substantial improvement in understanding the interior of the planet. Particularly we show that MORE can detect planetaryinduced librations allowing to constrain the size of a possible solid inner core inside the outer liquid core.

2017-04-01T00:00:00Z

['2017EGUGA..1917145J']

Contribution of BepiColombos MORE radio science experiment to the determination of Mercurys interior structure

['PUB_PDF']

2017EGUGA..1916026L

The COSIMA TOFSIMS spectrometer aboard Rosetta has collected nearly 40000 particles in orbit around 67PChuryumovGerasimenko from August 2014 to September 2016. These particles have been identified using the COSISCOPE optical microscope which imaged the 10 mm x 10 mm targets before and after exposure to the cometary environment with a resolution of 14 m pixel 1. Most of the particles in the smaller size ranges are fragments of larger parent particles 2. 4000 particles are resolved covering more than 2 pixels across and 550 particles are more than 100 m across 7 pixels which made it possible to characterize their typology using subpixel sampling 1. More than 90 of these large collected particles are aggregates pointing towards a high porosity low strength of the collected cometary material as discussed in 3. The optical properties of the collected particles provide supporting evidence that cometary material is dominated by high porosity low strength material most likely dominated by complex organic matter 4. Determining optical properties with COSISCOPE is a challenge as the LEDs on opposite sides of the target are set for providing high incidence 70 85 from the near to the far edge which means that relief slope is the major parameter controlling the signal from a particle. Several complementary approaches have been implemented. A small fraction of particlescover extended areas with low relief making it possible to directly infer the albedo by comparing the light level with that of neighbor substrate areas albedo measured in the lab 1.85 for gold black targets. For most particles one has to rely on the crossover of the light profiles from the left and right LEDs. With this approach the albedo of aggregates ranges from 2 to at most 20 and the relationship between the left and right profiles shows that photons penetrate 10s of m into such particles confirming a high porosity in line with the low strength. 1 Langevin et al. 2016 Typology of dust particles. Icarus 271 p. 76. 2 Merouane et al 2016 Dust particles flux and size distribution AampA doi 10.105100046361201527958 3 Hornung et al 2016 first assesment of the strength of cometary particles Planet. Space Sci. 133 p. 63 4 Fray et al 2016. highmolecular weight organic matter in cometary particles Nature 538 p. 72.

2017-04-01T00:00:00Z

['2017EGUGA..1916026L']

Optical properties of particles collected by COSIMA around 67PChuryumov Gerasimenko

['PUB_PDF']

2017EGUGA..1915162L

WAVEPAL is based on a general theory that we have developed for the frequency and wavelet analysis of irregularly sampled time series. It is based on the LombScargle periodogram that we extend to algebraic operators accommodating for the presence of a polynomial trend in the model for the data in addition to the periodic component and the background noise. Special care is devoted to the correlation between the trend and the periodic component. This new tool is then cast into the formalism of the Welch overlapping segment averaging WOSA method which is used to reduce the variance of the periodogramscalogram. We also design a test of significance against a background noise which is a continuous autoregressivemovingaverage CARMA Gaussian process. This widens the traditional choice of a Gaussian white or red noise process as the background noise. Estimation of CARMA parameters is performed in a Bayesian framework and relies on state of the art algorithms. We then provide algorithms computing the confidence levels for the periodogramscalogram that fully take into account the uncertainty on the CARMA noise parameters. Alternatively if one opts for the traditional choice of a unique set of parameters for the CARMA background noise we develop a theory providing analytical confidence levels which are more accurate than Markov chain Monte Carlo MCMC confidence levels and below some threshold for the number of data points less costly in computing time. We then estimate the amplitude of the periodic component with least squares methods and derive an approximate proportionality between the squared amplitude and the periodogramscalogram. The estimated signal amplitude also gives access to ridge filtering or filtering in a frequency band. Our results generalize and unify methods developed in the fields of geosciences engineering astronomy and astrophysics. WAVEPAL is written in python2.X and is available at httpsgithub.comguillaumelenoirWAVEPAL

2017-04-01T00:00:00Z

['2017EGUGA..1915162L']

WAVEPAL A Software for Frequency and Wavelet Analysis of Irregularly Sampled Time Series

['PUB_PDF']

2024PhRvC.109b5805T

We explore the influence of symmetry energy and the cut potential on the properties of pure nucleonic and hyperonrich neutron stars employing the relativistic meanfield RMF model with the S271 parameter set. The effects of symmetry energy are modulated by the SUBvSUB coupling while the cut potential is governed by the free parameter fSUBsSUB. The coupling constants between hyperons and mesons are ascertained based on the most recent hyperonnucleon potentials derived from existing experimental data. Our analysis suggests that SUBvSUB has more effect compared to fSUBsSUB on the composition and global properties of neutron stars. Our results are consistent with various observational data particularly with the GW170817 data.

2024-02-01T00:00:00Z

['2024PhRvC.109b5805T', '10.1103/PhysRevC.109.025805']

Influence of the symmetry energy and cut potential on the properties of pure nucleonic and hyperonrich neutron star matter

['PUB_HTML']

2017EGUGA..1916702G

Alberto GarcaRigo 1 David RomaDollase 2 Manuel HernndezPajares 1 Zishen Li 3 Michael Terkildsen 4 German Olivares 4 Reza GhoddousiFard 5 Denise Dettmering 6 Eren Erdogan 6 Haris Haralambous 7 Yannick Bniguel 8 Jens Berdermann 9 Martin Kriegel 9 Anna KrypiakGregorczyk 10 Tamara Gulyaeva 11 Attila Komjathy 12 Panagiotis Vergados 12 Joachim Feltens 1319 Ren Zandbergen 13 Tim FullerRowell 14 David Altadill 15 Nicolas Bergeot 16 Andrzej Krankowski 17 Loukis Agrotis 18 Ivan Galkin 20 Raul OrusPerez 21 1. UPCIonSAT research group Technical University of Catalonia Spain 2. Department of Engineering Electronics University of Barcelona UB Spain 3. Academy of OptoElectronics Chinese Academy of Sciences CAS China 4. Bureau of Meteorology Space Weather Services Australia 5. Canadian Geodetic Survey Natural Resources Canada NRCan Government of Canada Canada 6. Deutsches Geodtisches Forschungsinstitut der Technischen Universitt Mnchen DGFITUM Germany 7. Frederick University Cyprus Cyprus 8. IEEA France 9. Institute of Communications and Navigation DLR Germany 10. Institute of Geodesy UWM Poland 11. Institute of Terrestrial Magnetism ionosphere and Radio Wave Propagation Russian Academy of Sciences Russia 12. NASA Jet Propulsion Laboratory JPL California Institute of Technology USA 13. Navigation Support Office ESAESOC Germany 14. NOAA affiliate USA 15. Observatori de lEbre OE CSIC Universitat Ramon Llull 43520 Roquetes Spain 16. Planetology and Reference Systems Royal Observatory of Belgium ROB Belgium 17. Space RadioDiagnostics Research Centre UWM SRRCUWM Poland 18. SYMBAN Limited ESAESOC Germany 19. Telespazio VEGA Deutschland GmbH co ESAESOC Germany 20. University of Massachusetts Lowell Space Science Lab USA 21. Wave Interaction and Propagation Section TECEEP ESAESTEC The Netherlands IAGs Real Time Ionosphere Monitoring RTIM is a new Working Group within the International Association of Geodesy IAG SubCommission 4.3 Atmosphere Remote Sensing. The complementary expertise of the participating research groups allows to analyse the ionospheric behaviour from a broad perspective taking benefit of comparing multiple independent real time and near real time ionospheric approaches. In this context a detailed analysis will be presented for the days in March 2015 surrounding St. Patricks Day 2015 geomagnetic storm based on the existing ionospheric models global or regional within the group which are mainly based on Global Navigation Satellite Systems GNSS and ionosonde data. For this purpose a variety of ionospheric parameters will be considered including Total Electron Content TEC F2 layer critical frequency foF2 F2 layer peak hmF2 bottomside halfthickness B0 and ionospheric disturbance Windex. Also ionospheric highfrequency perturbations such as Travelling Ionospheric Disturbances TIDs scintillations and the impact of solar flares facing the Earth will be presented to derive a clear picture of the ionospheric dynamics. Among other sources of information to take part in the comparisons there will be 1 scintillation results from MONITOR ESAESTECfunded project derived by means of S4 index and Sigma Phi IEEA specially significant in the African sector and European high latitudes 2 dynamics of the global maps of Windex with 1h resolution derived from JPL Global Ionospheric Maps GIMs IZMIRAN 3 deviations from expected quiettime behavior analysed in terms of foF2 hmF2 B0 and B1 based on IRTAM and GIRO network of digisondes Lowell showing F2 layer peculiar changes due to the storm 4 statistics based on the median of the VTEC for the 15 previous days considering VTEC european regional maps ROB 5 time series of VTEC data that are derived by running the NRT ionosphere model of DGFITUM in offline mode which show clear variations for both global and European scales associated to the event 6 global maps of interfrequency phase rate variations as proxy phase scintillation index from 1Hz realtime IGS network NRCan 7 manually scaled ionospheric peak parameters from European ionosondes FUC 8 NOAA USTotal Electron Content Product NOAAUSTEC operational product which shows the passage of the stormenhanced density 9 as well as other products also from MONITOR ESAESTECfunded project such as the Rate of TEC index ROTI Single Receiver Medium Scale TIDs index SRMTID GNSS Solar Flare Detector GSFLAD which is a EUV rate proxy the Sunlit Ionosphere Sudden TEC Enhancement Detector SISTED and the Global Electron Content GEC generated from UQRG GIMs UPCIonSAT.

2017-04-01T00:00:00Z

['2017EGUGA..1916702G']

St. Patricks Day 2015 geomagnetic storm analysis based on Real Time Ionosphere Monitoring

['PUB_PDF']

2017CBET.4434....2W

The available astrometry the following elliptical orbital elements by G. V. Williams from 87 observations spanning Sept. 1129 and an ephemeris appear on MPEC 2017.S213. Epoch 2017 July 26.0 TT T 2017 July 28.0582 TT Peri. 99.9742 e 0.312971 Node 252.3863 2000.0 q 2.178983 AU Incl. 11.8532 a 3.171603 AU n 0.1744961 P 5.65 years

2017-09-01T00:00:00Z

['2017CBET.4434....2W']

Comet P2017 S5 Atlas

['PUB_HTML']

2024Mirro...7...33C

The NOIRLab component of the U.S. Extremely Large Telescope Program USELTP is steadily advancing towards its Conceptual Design Review by the U.S. National Science Foundation NSF in December 2024. Here we highlight recent progress in the technical development and community engagement aspects of the program.

2024-06-01T00:00:00Z

['2024Mirro...7...33C']

USELTP Moving Forward

['PUB_PDF']

2024JATIS..10c9002P

The goal of deformable mirrors DMs is to correct aberrated optical wavefronts in spaceborne electrooptical EO payloads. It is used as part of an activeadaptive optics system. A continuoussurface metalbased DM is highly reliable and less complex to assemble has better stability of the active surface is less expensive and can be manufactured quickly. In addition metal DM with actuation away from the active surface makes the overall configuration scalable. Continuing our previous work on deformable metal mirrors this work presents the design validation and qualification of an aluminum DM using 25 piezoelectric actuators which include an actuator in the center of the mirror to improve the spherical aberration correction accuracy. The optomechanical design and analysis of the deformable mirror assembly DMA are also presented for performance and survival loads. Later a qualification model QM was built with vacuumcompatible closedloop piezoelectric actuators. The correction accuracy was demonstrated at the QM by correcting aberrations in the mirror itself. The QM was successfully tested in the space environment in the ThermoVac for operating temperature limits of 20C5C and demonstrated survivability for storage temperature limits of 20C40C. Likewise the survivability of QM for launch environments such as sinusoidal and random vibration loads is demonstrated. The successful completion of all these tests has improved the maturity of this technology to the technology readiness level of 7 and is now ready to be configured for the appropriate spaceborne EO payload.

2024-07-01T00:00:00Z

['10.1117/1.JATIS.10.3.039002', '2024JATIS..10c9002P']

['mirror', 'correction accuracy', 'spherical aberration', 'qualification model', 'piezoelectric actuator', 'wavefront', 'optomechanical', 'root mean square']

Design and qualification of an aluminum deformable mirror for spaceborne electrooptical payloads

['PUB_HTML']

2014SPIE.9148E..51S

An adaptive optics system running at 1500 Hz was integrated using commercially available components. The deformable mirror was made by Alpao and has 277 actuators on a 15mm pitch. The wavefront sensor is based on the OCAM2 EMCCD Electronmultiplying chargecoupled device camera from First Light Imaging and a 2020 lenslet array. We present an initial system integration phase using the Alpao Core Engine toolbox running in a Matlab environment. During the second integration phase benchmark tests for Alpaos realtime controller ACEfast show the possibility to obtain a pure delay of 130 s in a parallel worker configuration with a computing power of 2 CPU8 core 4GPU for a problem size equivalent to stateoftheart adaptive optics systems.

2014-07-01T00:00:00Z

['10.1117/12.2056395', '2014SPIE.9148E..51S']

1500Hz adaptive optics system using commercially available components

['PUB_HTML']

2016xnnd.confE..67T

Powerful winds driven by active galactic nuclei AGN are often invoked to play a fundamental role in the evolution of both supermassive black holes SMBHs and their host galaxies quenching star formation and explaining the tight SMBHgalaxy relations. A strong support of this quasar mode feedback came from the recent Xray observation of a mildly relativistic accretion disk wind in an ultraluminous infrared galaxy and its connection with a largescale molecular outflow observed in the IR with Herschel suggesting a direct link between the SMBH and the gas out of which stars form. Spectroscopic observations especially in the Xray band suggest that such accretion disk winds may be common in local AGN and quasars. However their origin and characteristics are still not fully understood. Detailed theoretical models and simulations focused on radiation magnetohydrodynamic MHD or a combination of these two processes to investigate the possible acceleration mechanisms and dynamics of these winds. XMMNewton provided a fundamental contribution to these studies and it will still provide the highest effective area in the critical Fe K band of the spectrum until the launch of Athena. Very important improvements are expected from the high energy resolution of the Hitomi Xray Observatory.

2016-06-01T00:00:00Z

['2016xnnd.confE..67T']

Can supermassive black holes influence the evolution of their host galaxies

['PUB_PDF']

2016shin.confE.127Y

Modern observations are revealing the Suns largescale magnetic field to have a complex nonpotential structure. Moreover it is now widely believed that the loss of equilibrium of twisted magnetic flux ropes is responsible for many if not all coronal mass ejections. But predicting where these flux ropes will form and in particular whether or when they might erupt remains a challenge for model reconstructions of the coronal magnetic field. Recently we have identified the field line helicity is an appropriate and practical diagnostic for identifying twisted structures in coronal models. Since field lines are magnetic subdomains this is a more meaningful measure than the density of magnetic helicity at individual points. On the other hand it provides local information that the globallyintegrated magnetic helicity cannot. I will illustrate the power of this diagnostic on my own numerical nonpotential evolution model of the global corona.

2016-07-01T00:00:00Z

['2016shin.confE.127Y']

The Global Distribution of Magnetic Helicity in the Suns Corona

2016sofi.prop...38V

Magnetic fields permeate the Galactic ISM and have a significant influence on the formation of molecular clouds and stars. Farinfrared polarization from thermal dust grains aligned with the fields provides the strongest method for mapping the magnetic field strength and orientation. However the exact method of grain alignment is still a matter of debate that thus leaves ambiguity in determination of where along the lineofsight polarization can reliably trace the field. The observations proposed here aim to improve that degeneracy by testing models of grain alignment which can then identify environmental conditions in which the field measurements are most reliable. Key predictions of grain alignment models lead to characteristic spectral shapes with strong variations in the FIR. We propose to test these predictions with multiwavelength observations of the total polarized and unpolarized intensity in numerous environments e.g. HII regions and hot protostellar cores. The primary measurements are multiwavelength maps of total intensity polarized intensity and polarization position angle in three Galactic molecular clouds on scales of several arcminutes with high resolution 519 arcsec. From the multiwavelength maps this work will generate polarization spectra at pointbypoint locations in each cloud. At a minimum this will characterize the FIR polarization spectra as a function of environment for the first time and more broadly provide input to test models of grain alignment. The maps will also measure the magnetic field morphology in cloud regions of the hottest dust complementing longer wavelength measurements in cooler dust.

2016-01-01T00:00:00Z

['2016sofi.prop...38V']

['SOFIA 05_0038']

Characterizing the FIR polarization spectrum in Galactic Clouds

2016sofi.prop...36C

We propose higher angular resolution HAWC Dband and deeper polarimetric observations twice the integration time than the tabulated ROC plan for the dense core of the nearby 140 pc dark cloud L1544. We will use these data to test ambipolar diffusion models of this prestellar core and to critically compare HAWC polarimetric maps to our nearinfrared background starlight polarimetry and reprocessed SCUPOL map of the Bfield of this cloud. Further we propose sensitive HAWC Eband polarimetric observations of the outer more diffuse pair of cloud cores L1544 E and L1544 W located outside the ROC FOV. These HAWC data will permit comparing how the Bfield strengths from the ChandrasekharFermi method vary with radial offset for the diffuse and dense cores. All of these data taken together will permit quantitative comparisons of position angle structure functions to assess the ratio of random to uniform Bfield strengths in each core.

2016-01-01T00:00:00Z

['2016sofi.prop...36C']

['SOFIA 05_0036']

The Magnetic Fields of the Dense and Diffuse Cores in L1544

2016cxo..prop.4896K

We will use the LETG to characterize the EUVemitting boundary layer BL and disk wind of two dwarf novae in outburst. These data will allow us to test stateoftheart BL models determine the outflow geometry and kinematics and characterize the aperiodic EUV variability. However the program is also a pathfinder for the Great Observatories Accretion Legacy Survey. GOALS is a planned multiwavelength campaign that will follow a dwarf nova through an entire outburst with nearcontinuous coverage from Xrays to radio. This campaign will provide an unprecedented view of transient disk accretion and will become the benchmark for theoretical models. Our targets are the best candidates for GOALS but LETG observations are required to confirm their viability.

2016-09-01T00:00:00Z

['2016cxo..prop.4896K']

EUV Emission from Accreting White Dwarfs in Outburst A Pathfinder for the Great Observatories Accretion Legacy Survey

2016cosp...41E1776S

Signatures of the seismic activity in the ionospheric F2 region have been studied by analyzing the measurement of electron and ion temperatures during the occurrence of earthquake. The ionospheric electron and ion temperatures data recorded by the RPA payload aboard the Indian SROSSC2 satellite during the period from January 1995 to December 2000 were used for the altitude range 430630 km over Indian region. The normal days electron and ion temperatures have been compared to the temperatures recorded during the seismic activity. The details of seismic events were obtained from USGS earthquake data information website. It has been found that the average electron temperature is enhanced during the occurrence of earthquakes by 1.2 to 1.5 times and this enhancement was for ion temperature ranging from 1.1to 1.3 times over the normal days average temperatures. The above careful quantitative analysis of ionospheric electron and ion temperatures data shows the consistent enhancement in the ionospheric electron and ion temperatures. It is expected that the seismogenic vertical electrical field propagates up to the ionospheric heights and induces Joule heating that may cause the enhancement in ionospheric temperatures.

2016-07-01T00:00:00Z

['2016cosp...41E1776S']

Ionospheric Response Due to Seismic Activity

2016cosp...41E1778S

The Stratospheric Sudden Warming SSW is one of the most spectacular phenomena in the atmosphere and has impacts on the Earths lower middle and upper atmospheres. Lidar is one of the best instrument to study Earths middle atmospheric thermal structure with very temporal and vertical resolution. A Nd YAG laser based Rayleigh Lidar is operational over Mt. Abu India 24.5 oN 72.7 oE since 1997.In this study two major SSW episodes associated with vortex displacement and vortex splitting occurred in year 1998 and 1999 respectively are investigated first time over Mt. Abu using lidar observations. Analyses show that CIRA86 and MSISE90 model fail to capture these SSW episode whereas ground based lidar and satellite observations from Halogen occultation experiment HALOE onboard upper atmospheric research satellite UARSare able to capture effect of SSW events. Lidar measurements are able to capture SSW warming and its decay very accurately. Impact of SSW is further investigated in ECMWF Interim reanalyzed potential vorticity. Moreover a detail study has been presented to understand the latitudinal variation of SSW warming and associated mesospheric cooling over Indian region.

2016-07-01T00:00:00Z

['2016cosp...41E1778S']

Analysis of Stratospheric Sudden Warming SSW over Tropical and Subtropical Regions of India using Rayleigh Lidar and Satellite measurements

2016cxo..prop.4994H

Chandra Xray surveys have revolutionized our view of the growth of black holes across cosmic time. Recently fundamental questions have emerged about the connection of AGN to their host large scale structures that clearly demand a wide deep survey over a large area comparable to the recent extensive Chandra surveys in smaller fields. We propose the Chandra Deep WideField Survey CDWFS covering the central 6 sq. deg in the Bootes field totaling 1.025 Ms building on 550 ks from the HRC GTO program. CDWFS will efficiently probe a large cosmic volume allowing us to carry out accurate new investigations of the connections between black holes and their largescale structures and will complete the next generation surveys that comprise a key part of Chandras legacy.

2016-09-01T00:00:00Z

['2016cxo..prop.4994H']

The Chandra Deep WideField Survey Completing the new generation of Chandra extragalactic surveys

2016csss.confE..57B

The 32 Ori moving group was discovered almost a decade ago and despite the fact that it represents thefirst northern young 20 Myr stellar aggregate within 100 pc of the Sun a comprehensive characterisationof the stellar content of the group has yet to be performed. We hereby present the first largescalespectroscopic survey for new predominantly lowmass K and Mtype members of the 32 Ori moving groupafter combining kinematic and photometric data to select candidate members with Galactic space motionand positions in colourmagnitude space consistent with group membership. Final memberships are assignedon the basis of a combination of radial velocity H emission and Li absorption diagnostics. Weidentify 25 new members thereby increasing the number of known 32 Ori moving group members by a factorof 3. Finally we demonstrate consistent ages for the group based on isochronal fitting in thecolourmagnitude diagram and the location of the Li depletion boundary. This consistency suggests thatthe group is essentially coeval with the Beta Pictoris moving group with an age in the range 2025 Myr.In the era of SPHERE GPI ALMA etc. this group therefore represents a benchmark region for directimagingstudies of circumstellar disc evolution especially during the epoch of terrestrial planet formation andof course extrasolar planets.

2016-06-01T00:00:00Z

['10.5281/zenodo.56486', '2016csss.confE..57B']

['stars: kinematics', 'stars: pre-main-sequence', 'open clusters and associations: individual: 32 Ori', 'techniques: spectroscopy', 'Zenodo community cs19']

A Stellar Census Of The 32 Ori Moving Group

['PUB_HTML']

2016cosp...41E2166Z

BeiDou Navigation Satellite System BDS does not have the ability of global navigation and positioning currently. The whole tracking observation of satellite orbit and the geometry of reference station are not perfect. These situations influence the accuracy of satellite orbit determination. Based on the theory and method of dynamic orbit determination the analytical contribution of multiGNSS combined orbit determination to the solution precision of parameters was derived. And using the measured data the statistical contribution of BDSGPS combined orbit determination to the solution precision of orbit and clock error was analyzed. The results show that the contribution of combined orbit determination to the solution precision of the common parameters between different systems was significant. The solution precisions of the orbit and clock error were significantly improved except GEO satellites. The statistical contribution of BDSGPS combined orbit determination to the precision of BDS satellite orbit the RMS of BDS satellite clock error and the RMS of receiver clock error were 36.21 26.88 and 20.88 respectively. Especially the contribution to the clock error of receivers which were in the area with few visible satellites was particularly significant. And the statistical contribution was 45.95.

2016-07-01T00:00:00Z

['2016cosp...41E2166Z']

Contribution Analysis of BDSGPS Combined Orbit Determination

2016cxo..prop.4989P

Cas A is one of only a handful of young supernova remnants to exhibit time variations in thermal and nonthermal emission and is the only remnant to show evidence for an evolving young central neutron star. Here we propose to continue our multicycle monitoring program with three 50 ksec observations of Cas A spaced by approximately one year which are designed to 1 probe the structure and composition of supernova ejecta by following its evolution as it is heated by the reverse shock 2 test theories of particle acceleration at supernova shocks and 3 monitor the surface temperature evolution of the neutron star to test theories of nuclear and condensed matter physics and in particular superfluidity and superconductivity.

2016-09-01T00:00:00Z

['2016cxo..prop.4989P']

Continued Multicycle Monitoring of the Young Galactic Supernova Remnant Cassiopeia A

2016cosp...41E2164Z

Ionizing radiation and microgravity were considered to be the most important stress factors of space environmental the respective study of the biological effects of the radiation and microgravity carried out earlier but the interaction of the effects of radiation with microgravity started later and due to difference of the materials and methods the result of this experiment were not consistent. To further investigate the influence of microgravity on the expression of the radiation damage repair genes the seed of Arabidopsis Col and its gravityinsensitive mutant PIN2 were exposed to 0.1Gy of the dose of energetic carbonion beam radiation LET 30KeV m and the germinated seed were than fixed in the 3D random positioning apparatus immediately for a 10day simulated microgravity. By measuring the deflection angle of root tip and the changes of the expression of Ku70 and RAD51 protein we investigated the impact of microgravity effect on radiation damage repair systems. The results shown that radiation microgravity and microgravity with radiation could increase the angle of the root of the Col significantly but no obvious effect on PIN2 type. The radiation could increase the expression of Ku70 significantly in both Col and PIN2 microgravity does not affect the expression but the microgravity with radiation could decrease the expression of Ku70. This result shown that the microgravity could influence the radiation damage repair systems in molecular level. Moreover our findings were important to understand the molecular mechanism of the impact of microgravity effect on radiation damage repair systems in vivo.

2016-07-01T00:00:00Z

['2016cosp...41E2164Z']

Simulated microgravity influenced the expression of DNA damage repair genes

2016cosp...41E1867S

The DArk Matter Explorer DAMPE is a satellite based experiment aiming for dark matter search and many other topics astronomy interested. The Plastic Scintillator Detector PSD gives DAMPE the ability to measure charge of the crossing particles and separate gamma from electrons which are necessary for achieving the goals of the experiment. The PSD is composed by 82 scintillator counters and read at both ends by a total of 162 photomultiplier tubes. In this paper we describe the final design of DAMPEPSD the expected performances and shows some results of the beam test carried on at CERN.

2016-07-01T00:00:00Z

['2016cosp...41E1867S']

The Plastic Scintillator Detector of the DAMPE space experiment

2016cosp...41E2066W

The CassiniHuygens mission is entering its final phase. The landing of Huygens on Titan and flybys performed by the Cassini probe during the last ten years revolutionized our knowledge about that moon revealing a complex fluviolacustrine environment. Despite significant differences in composition temperature and gravity the processes of sediment transport and deposition are similar on Earth and Titan. We performed numerical simulations of development of river deltas in Titanian and terrestrial conditions under various discharges and with different dominant grain sizes. We found that evolution of deltaic deposits is more rapid on Titan due to higher efficiency of transport but the flat lobate river deltas may form in narrower range of parameters than on Earth. Our results help in understanding the evolution of sedimentary deposits and may partially explain the paucity of river deltas in Titans lakes.

2016-07-01T00:00:00Z

['2016cosp...41E2066W']

Morphology of river deltas on Titan and Earth

2016cosp...41E2064W

We use observations from the MESSENGER spacecraft in orbit around Mercury to investigate interplanetary coronal mass ejections ICMEs near 0.3 AU. MESSENGER is the first spacecraft since Helios 1 and 2 in the 1980s to make in situ measurements of the interplanetary medium at heliocentric distances lt 0.5 AU. Because extensive observations both remote sensing and insitu are available throughout the MESSENGER mission these data present a unique opportunity for observing the innermost heliosphere and the development of the solar wind and interplanetary transients. We catalog ICME events observed by the MESSENGER Magnetometer between 2011 and 2015 and present statistical analyses of ICME properties at Mercury. In addition using existing data sets of ICMEs at 1 AU we investigate key ICME property changes from Mercury to 1 AU. Using our database of nearly 70 ICMEs we also statistically characterize Mercurys magnetosphere during times of ICMEs when Mercurys magnetosphere becomes significantly altered. We conduct a systematic investigation of the largescale processes in Mercurys magnetosphere during extreme solar wind conditions by studying the motion of the bow shock and magnetopause boundaries erosion of the dayside magnetosphere the size extent and plasma pressure of the cusp region and the plasma precipitation to the surface.

2016-07-01T00:00:00Z

['2016cosp...41E2064W']

Interplanetary coronal mass ejections at Mercury Database and effects on the magnetosphere

2016shin.confE.119M

Magnetic topology is a powerful tool for describing the structure of magnetic fields during three dimensional reconnection. The bifurcation of magnetic null points is one of the most important ways by which magnetic topology can evolve. However most studies on null point bifurcation take an analytical approach that neglects the effects of feedback from nonideal plasmas e.g. Murphy et al. 2015. We review what is currently known about three dimensional magnetic null points and the evolution of their magnetic skeletons. We also outline the plans and preliminary results for a detailed localized numerical simulation of bifurcating null points using resistive MHD.

2016-07-01T00:00:00Z

['2016shin.confE.119M']

Null Point Bifurcations During 3D Magnetic Reconnection

2016cosp...41E1866S

Ionizing radiation IR is a known mutagen responsible for causing DNA strand breaks in all living organisms. Strand breaks thus created can be repaired by different mechanisms including homologous recombination HR one of the key mechanisms maintaining genome stability. Here we used previously generated Arabidopsis thaliana transgenic for homologous recombination reporter system in which homologous recombination frequencyHRF was used as mutagenic end points. Based on the system effect of DNA damage by spaceflight during the Shenzhou9 mission was investigated and the results showed that 13 days spaceflight exposure of seedlings induced a significant increase in HRF compared with its groundbase threedimensional clinostat controls and ground 1g controls. We also observed threedimensional clinostat induced a significant increase in HRF compared with ground 1g controls. Molecular hydrogen H2 has antioxidant activities by selectively reducing hydroxylradical OH and peroxynitriteONOO so we investigated the effect of hydrogen on IRinduced HRF. Treatment with hydrogenrich water dramatically reduced the HR frequency induced by exposure of seedlings to 0 to 80 Gy 60Co radiation suggesting that hydrogen represents a potentially novel preventative strategy for radiationinduced DNA damage in plants.

2016-07-01T00:00:00Z

['2016cosp...41E1866S']

The study on spaceflight induced DNA damage in Arabidopsis thaliana and the protective effect of hydrogen

2016cosp...41E1865S

We address the problem of determining the limiting energetic ring current ion spectrum resulting from electromagnetic ion cyclotron EMICwaveioninteractions. We solve the problem in a relativistic regimeincorporating a cold background multiion plasma component and without assuming a predetermined form for the particle energy distribution. The limiting spectrum is determined by the condition that the EMIC waves acquire a certain gain over a given convective length scale for all frequencies over which wave growth occurs. We find that the limiting ion spectrum satisfies an integral equation that must be solved numerically. However at large particle energy E the limiting spectrum varies simply as 1E. Moreoverthis spectral shape does not depend on the energetic ion in question nor on the background multiion plasma composition. We provide numerical solutions for the limiting spectra for Earthlike parameters and we compare measured ion spectra from the Van Allen Probes with corresponding numerical limiting spectra.

2016-07-01T00:00:00Z

['2016cosp...41E1865S']

Energetic ring current ion spectra shaped by EMIC wave scattering loss

2016gac..conf..317R

Solution of the small value of the cosmological constant problem is presented based on multidimensional gravity.

2016-01-01T00:00:00Z

['2016gac..conf..317R', '10.1142/9789814759816_0068']

Spacetime foam and the cosmological constant problem

['PUB_HTML', 'PUB_PDF']

2016diga.confE...3R

I review some of the mechanisms coupling disk dynamics to the scale of star cluster formation. In particular I show how the complex structure of the bar both triggers the formation of massive cluster and regulates the formation of star in the innermost regions. I also discuss the effect of stellar feedback in affecting scales larger than the star forming clouds themselves.

2016-10-01T00:00:00Z

['10.5281/zenodo.163104', '2016diga.confE...3R']

['Discs in galaxies', 'Zenodo community discs2016']

Star Formation Regulated By Disk Dynamics

['PUB_HTML']

2016xmm..prop..158B

Central Compact Objects CCOs are a handful of faint and young Xrayemitting neutron stars at the center of bright supernova remnantsusually lacking detection at any other wavelength. So far only eightsources are classified as CCOs. Three of them are known to be neutronstars with periods in the range 0.10.4 s and dipolar magnetic field ofthe order of 1e101e11 G while one has instead an extremely slow spinperiod of about 6.7 hr and a few others do not show pulsations. CXOUJ181852.0150213 is a proposed CCO candidate. We request to observethis source with XMMNewton for the first time with a total exposuretime of 130 ks in order to properly characterize its spectral and timingproperties looking for spectral lines and Xray pulsations.

2016-10-01T00:00:00Z

['2016xmm..prop..158B']

Unveiling the Central Compact Object nature of CXOU J181852.0150213

2016yCat..51520075O

Our survey instrument nicknamed AggieCam consists of an Apogee Alta F16M camera with a 40964096pixel Kodak KAD16083 CCD that is thermoelectrically cooled down to T45C relative to ambient. Testing of the CCD showed a dark current of 0.2eSUPSUPpixs at temperatures of 25C relative to ambient. The optics include a Mamiya photographic 300mm lens with a Hoya UV and IR cut filter to restrict the wavelength range to 0.40.7m. The effective aperture size of the telescope is 53.6mm and the total throughput of the system is near 45. The pixel scale of the detector is 6.2pix leading to a total field of view hereafter FOV of 50degSUP2SUP. The telescope was installed at the Estacion Astrofisica de Bosque Alegre hereafter EABA as part of an ongoing collaboration with the Universidad Nacional de Cordoba which owns and operates the site. P EABA is a research and outreach observatory located at 31.412S 64.489W at an altitude of 1350m 50km from the city of Cordoba province of Cordoba Argentina. Nearly all observations were carried out remotely from the Mitchell Institute of Fundamental Physics and Astronomy at Texas AampM University in College Station Texas. Logistical support for the instrument was provided by staff members of the Instituto de Astronomia Teorica y Experimental Observatorio de Cordoba and EABA. P We targeted three young stellar associations to maximize the science return from our study IC 2391 8SUPhSUP40SUPmSUP53 the eta Chamaeleontis cluster etaCha8SUPhSUP45SUPmSUP79 and the Upper Scorpius association USco16SUPhSUP24.5. P Any transiting Hot Jupiter HJ or premainsequence eclipsing binary PMB candidate passing all of the significance tests described in Sections 4.1 and 4.2 was then subject to a series of follow up photometric observations. The 1.54m telescope at EABA provided 300hr of BVRI photometry to date with further observations planned. The 0.8m telescope at the McDonald Observatory provided 14hr of BVRI photometry. The Las Cumbres Global Observatory Telescope Network LCOGT provided 30hr of gri photometry from their 1m facilities. The Texas AampM University campus observatory 0.5m telescope provided 30hr of gri photometry. Additionally the 2.1m telescope at the McDonald Observatory coupled with the Sandiford Echelle Spectrograph provided 14hr of initial spectroscopic follow up during the Spring of 2015. P 3 data files.

2016-09-01T00:00:00Z

['2016yCat..51520075O', '10.26093/cds/vizier.51520075']

['Associations: stellar', 'Clusters: open', 'Stars: variable', 'Binaries: eclipsing', 'Stars: pre-main sequence', 'Stars: nearby', 'Stars: double and multiple', 'Planets']

VizieR Online Data Catalog Photometric survey of IC 2391 eta Cha and USco Oelkers 2016

['PUB_HTML']

2016xnnd.confE..82C

High energy studies of astrophysical dust complement observations of dusty interstellar gas at other wavelengths. With high resolution Xray spectroscopy dust scattering significantly enhances the total extinction optical depth and alters the shape of photoelectric absorption edges. This effect is modulated by the dust grain size distribution spatial location along the line of sight and the imaging resolution of the Xray telescope. At soft energies the spectrum of scattered light is likely to have significant features at the 0.3 keV CK 0.5 keV OK and 0.7 keV FeL photoelectric absorption edges. This direct probe of ISM dust grain elements will be important for i understanding the relative abundances of graphitic grains or PAHs versus silicates and ii measuring the depletion of gas phase elements into solid form. We focus in particular on the FeL edge fitting a template for the total extinction to the high resolution spectrum of three Xray binaries from the Chandra archive GX 99 XTE J1817330 and Cyg X1. We discuss ways in which spectroscopy with XMM can yield insight into dust obscured objects such as stars binaries AGN and foreground quasar absorption line systems.

2016-06-01T00:00:00Z

['2016xnnd.confE..56C', '2016xnnd.confE..82C']

The effects of dust scattering on highresolution Xray absorption edge structure

['PUB_PDF']

2016yCat..17830004W

Our sample consists of bright host stars with multiplanet transiting systems from Kepler. Out of 5779 Kepler Objects of Interest httpexoplanetarchive.ipac.caltech.edu we selected all the systems with a Kepler magnitude KSUBPSUB brighter than 13.5mag and with at least two planet candidates. The sample includes 343 planet candidates see Table3 in 138 multiplanet candidate systems see Table2 from the Kepler mission. For these systems we used archival data from Kepler to characterize their stellar see Table2 and orbital properties see Table3. We used UKIRT images to calculate brightness contrast curves and to detect stellar companions around planet candidate host stars see Table4. P 3 data files.

2016-05-01T00:00:00Z

['2016yCat..17830004W', '10.26093/cds/vizier.17830004']

['Stars: double and multiple', 'Planets', 'Stars: masses', 'Effective temperatures', 'Abundances: [Fe/H]', 'Stars: diameters']

VizieR Online Data Catalog Properties of Kepler multiplanet candidate systems Wang 2014

['PUB_HTML']

2016xmm..prop...89S

Fermi has detected over 200 gammaray pulsars of varying types in 8 yearsof operations but the socalled soft lt 100 MeV gammaray pulsarsremain relatively elusive. Typically singlepeaked younger and moreenergetic than GeV pulsars such pulsars were particularly hard to detectwith Fermi prior to the release of Pass 8. Increasing the size of thispopulation may shed light on our current understanding of highenergypulsars and the effect that various parameters e.g. geometry may haveon the observed emission. We propose short 5ks XMM observations of ourtop 5 soft gammaray pulsar candidates to enable the first sensitiveblind searches for such pulsars using LAT data below 100 MeV.

2016-10-01T00:00:00Z

['2016xmm..prop...89S']

Searching for soft gammaray pulsars in unassociated Fermi LAT sources with

2016wfc..rept....8B

The Wide Field Camera 3 WFC3 UVIS detector possesses an intrinsic signal during exposures even in the absence of light known as dark current. A daily monitor program is employed every HST cycle to characterize and measure this current as well as to create calibration files which serve to subtract the dark current from science data. We summarize the results of the daily monitor program for all onorbit data. We also introduce a new algorithm for generating the dark reference files that provides several improvements to their overall quality. Key features to the new algorithm include correcting the dark frames for Charge Transfer Efficiency CTE losses using an annealcycle average value to measure the dark current and generating reference files on a daily basis. This new algorithm is part of the release of the CALWF3 v3.3 calibration pipeline on February 23 2016 also known as UVIS 2.0. Improved dark reference files have been regenerated and redelivered to the Calibration Reference Data System CRDS for all onorbit data. Observers with science data taken prior to the release of CALWF3 v3.3 may request their data through the Mikulski Archive for Space Telescopes MAST to obtain the improved products.

2016-04-01T00:00:00Z

['2016wfc..rept....8B']

['Hubble Space Telescope', 'HST', 'Space Telescope Science Institute', 'STScI', 'WFC3', 'UVIS', 'calibration']

WFC3UVIS Dark Calibration Monitoring Results and Improvements to Dark Reference Files

['PUB_PDF']

2016xmm..prop...80T

During outbursts black hole BH transients enter into different spectralstates depending on the mass accretion rate as well as at least one otherphysical parameter. Although we do not know which second parameter ismost important candidates include jet power disk viscosity which maybe related to magnetic field generation and transport and inner diskradius. The recurrent 20 outbursts to date BH transient 4U 163047usually exhibits different state evolution than other systems. Inparticular during outburst decay we found that its spectrum canremain soft down to very low luminosity and this may indicate a lowdisk viscosity. We propose an XMM TOO to constrain the origin of thelowsoft state emission which has implications for the disk geometryand viscosity.

2016-10-01T00:00:00Z

['2016xmm..prop...80T']

The Black Hole Transient 4U 163047 in the LowSoft State

2016wfc..rept....4M

An improved set of flat fields was delivered to the HST archive on February 23 2016 as part of the UVIS 2.0 photometric calibration. This new methodology treats the two UVIS chips as separate detectors when computing the flats and zeropoints. The most significant difference in the new flats is that each chip is now normalized by its median value removing any inherent sensitivity offsets from the flats themselves. Instead the new software CALWF3 version 3.3 corrects for this effect by scaling the UVIS2 science extension by the sensitivity ratio between chips as determined from observations of white dwarf standards. For the majority of filters the maximum change in the flat field is less than 1. For the UV filters the flats are based on ground test data obtained in ambient conditions. These have been updated to correct for 3 sensitivity variations in a crosshatch pattern on scales of 50100 pixels across both chips. To improve cosmetics in calibrated images the new flats contain additional corrections for bad rows and columns and new data quality flags for slight vignetting in the outer corner of UVIS1 amp A.

2016-03-01T00:00:00Z

['2016wfc..rept....4M']

['Hubble Space Telescope', 'HST', 'Space Telescope Science Institute', 'STScI', 'WFC3', 'UVIS', 'flat fields', 'photometry', 'repeatability']

UVIS 2.0 ChipDependent Flats

['PUB_PDF']

2016xmm..prop...81A

The discovery of bright ringlike Xray emission at the heart of thelarge supernova remnant SNR HB3 has invoked many possible explanationsfor this unique morphology including a second SNR a presupernovacircumstellar shell or an unusual density distribution. Howeverprevious observations of this remnant have either suffered fromsignificant flaring or were taken by low spatial and spectralresolution instruments. This makes it difficult to characterise theproperties of this central emission and determine the origin of thisunique morphology. Here we propose two XMMNewton observations ofthe heart of HB3 to map its bright central emission and some of itsdiffuse surroundings in an attempt to shed light on origin and naturethis structure.

2016-10-01T00:00:00Z

['2016xmm..prop...81A']

A ring around the heart of supernova remnant HB3

2016yCat..18149006R

We measure the equivalent widths of Ly and the C III doublet in the restframe UV spectra of 11 gravitationally lensed galaxies at 1.6ltzlt3.1. Spectra were obtained using the MagE spectrograph on the Clay Magellan II telescope as part of a large study of the restframe ultraviolet spectral properties of bright lensed galaxies J. R. Rigby et al. 2016 in preparation. We also take C III equivalent widths from literature see section 2. P 1 data file.

2016-03-01T00:00:00Z

['10.26093/cds/vizier.18149006', '2016yCat..18149006R']

['Galaxies: nearby', 'Equivalent widths', 'Gravitational lensing']

VizieR Online Data Catalog CIII emission in near amp far starforming galaxies Rigby 2015

['PUB_HTML']

2016yCat..35930007H

Column density NSUBHSUB and extinction ASUBVSUB values are sample of YSO sources in the ONC. Nearinfrared colours based on the VISION Meingast et al. 2016AampA...587A.153M catalogue were employed to calculate extinction values using the NICER algorithm Lombardi et al. 2001AampA...377.1023L and assuming RSUBVSUB3.1. Column densities were adopted from the COUP Getman et al. 2005 Cat. JApJS160319 catalogue. In addition to NSUBHSUB and ASUBVSUB the following quantities are provided JHKs magnitudes taken from the VISION catalogue spectral types adopted from the catalogue by Hillenbrand et al. 2013 Cat. JAJ14685 intrinsic nearinfrared colours deduced from spectral types and data by Scandariato et al. 2012AampA...545A..19S and the YSO classification based on the classification by Megeath et al. 2012 Cat. JAJ144192. 1Sigma error estimates are given for all quantities in the table. P 1 data file.

2016-07-01T00:00:00Z

['10.26093/cds/vizier.35930007', '2016yCat..35930007H']

['Extinction', 'Infrared sources', 'X-ray sources', 'YSOs']

VizieR Online Data Catalog NH and AV Towards YSOs in the ONC Hasenberger 2016

['PUB_HTML']

2016yCat..51500200H

Cz 30 was observed using the WisconsinIndianaYaleNOAO WIYN 0.9m telescope with the S2KB imager a 20482048 pixel CCD with a pixel scale of 0.6pixel providing a total field of view of 20.520.5. Observations were taken on 2012 February 17 in B V and I filters with a typical seeing of about 1.5 and the CCD centered near the cluster center. We present our set of photometry in Table3. P Cz 30 was also observed with the Hydra multiobject fiber positioner and Bench Spectrograph on the WisconsinIndianaYaleNOAO WIYN 3.5m telescope. The cluster was observed on 2014 January 18 and 19 and February 14 UT in the echelle mode giving a dispersion of 0.16pixel and covering the range of 60606380. Table4 gives the results of velocity determinations for stars in Cz 30. P Table5 gives lines used along with the measured equivalent widths. We obtained FeH estimates for 10 stars whose final atmospheric parameters and abundances are given in Table6. P 4 data files.

2016-06-01T00:00:00Z

['2016yCat..51500200H', '10.26093/cds/vizier.51500200']

['Clusters: open', 'Photometry: UBVRI', 'Equivalent widths', 'Radial velocities', 'Effective temperatures', 'Abundances: [Fe/H]']

VizieR Online Data Catalog Photometry and spectroscopy of stars in Cz 30 Hayes 2015

['PUB_HTML']

2016yCat.2042....0H

A narrowband spectrometer compensated for seeing and transparency variations has been constructed and used to measure the strength of the calcium Kline 3933.68 in 146 Atype stars. The observations were made in the spring of 1966 with the No.4 16inch 40cm telescope at Kitt Peak National Observatory. P 1 data file.

2016-11-01T00:00:00Z

['2016yCat.2042....0H']

['Photometry: K-line', 'Stars: A-type']

VizieR Online Data Catalog KLine Photometry of A Stars Henry 1969

2016yCat..17820045D

All the spectroscopy and imaging observations reported here were obtained with the ShangriLa telescope SLT IAU site code O44 at the Lijiang Station of the Yunnan Observatory of the Chinese Academy of Sciences. The SLT started its operation in 2008. This is a 2.4m altazimuth mounted RitcheyChretien telescope. The rms pointing error is about 2arcsec rms and the tracking accuracy with autoguiding is better than 0.5hr. The longitude of the station is 1000151E the latitude 264232N and the altitude 3193m. The annually averaged seeing is 1.5 in terms of the FWHM of stars measured with Yunnan Faint Object Spectrograph and Camera YFOSC ranging from 0.7 to 2.0. P The YFOSC built in 2010 by the astronomical instrumentation team at the Niels Bohr Institute is similar to the ESO Faint Object Spectrograph and Camera but with an additional focal reducer. It started its operation in 2011. YFOSC is a versatile instrument for low resolution spectroscopy and imaging working at the Cassegrain focus. The CCD chip is an e2v CCD4290 Back Illuminated Deep Depletion 20484608 pixel Scientific CCD Sensor whose pixel size is 13.5mm pixel scale 0.283pixel covering a 1010 field of view FOV. P Our Reverberation Mapping RM campaign started in 2012 October. All the spectra were obtained using YFOSC with Grism 14 which provides a resolution of 92mm 1.8pixel and covers the wavelength range of 38007200. P In this first paper of the series we report the observations of three objects Mrk 142 Mrk 335 and IRAS F123973333. P 3 data files.

2016-03-01T00:00:00Z

['2016yCat..17820045D', '10.26093/cds/vizier.17820045']

['Active gal. nuclei', 'Galaxies: Seyfert', 'Accretion', 'Spectroscopy']

VizieR Online Data Catalog SEAMBHs. I. Mrk 142 Mrk 335 and IRAS F123973333 Du 2014

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2016xnnd.confE..21H

The Cherenkov Telescope Array CTA is a nextgeneration observatory for very high energy VHE gammaray astronomy. With one array of imaging atmospheric Cherenkov telescopes each in the northern and southern hemispheres CTA will provide fullsky coverage enhance flux sensitivity by one order of magnitude compared to current instruments cover gammaray energies from 20 GeV to 300 TeV and provide angular resolution of a few arcminutes across a multidegree field of view. In the context of its Key Science Projects KSPs CTA will conduct a census of particle acceleration in the universe with quartersky extragalactic fullplane Galactic and Large Magellanic Cloud surveys planned. Additional KSPs are focused on transients acceleration up to PeV energies in our own galaxy active galaxies starforming systems on a wide range of scales and the Perseus cluster of galaxies. A major element of the programme is the search for dark matter in particular the annihilation signature of WIMPs. Like for currentgeneration VHE instruments CTA science will strongly rely upon multiwavelength observations of sources with the Xray domain playing a particularly crucial role. The presentation will briefly introduce CTA summarize its science perspectives and address the synergies with instruments in other wavebands.

2016-06-01T00:00:00Z

['2016xnnd.confE..21H']

Synergies with CTA and VHE Astrophysics

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2016yCat..51500191R

Nearinfrared images of the CygnusX DR15 region were obtained with the OMEGA 2000 camera at the 3.5m telescope of the Calar Alto Observatory atop Sierra de los Filabres in Almeria Spain during the nights of 2010 February 2nd and March 3rd. The data set consists of 900s coadded exposures in the J H and K bands 1.209 1.648 and 2.208m respectively. The seeing valuesmeasured directly from the average FWHM of stars in the final reduced mosaicswere 1.17 1.13 and 0.98 in J H and K respectively. P The Spitzer Space Telescope has observed the DR15 cluster with the IRAC and MIPS detectors as part of the Spitzer CygnusX Legacy Survey Hora et al. 2009 ASP Conf. Ser. Reionization to Exoplanets Spitzers Growing Legacy ed P. Ogle San Francisco CA ASP 26 hereafter CXLS. We obtained archival enhanced product mosaics from the Spitzer Heritage Archive as well as a photometric catalog coincident with our region of interest directly from the CXLS Data Release 1 DR1. The catalog contains calibrated magnitudes for sources detected with IRAC in its four cryogenic mission channels 3.6 4.5 5.8 and 8.0m as well as in the 24m channel of MIPS. P The DR15 cluster was observed with the Imaging Array of the Chandra Advanced CCD Imaging Spectrometer ACISI on 2011 January 25 ObsID12390 P.I. Wright. P We made use of the Five College Radio Observatory FCRAO SUP13SUPCO10 molecular radio emission map of the south CygnusX region from the study of Schneider et al. 2011AampA...529A...1S. P In Tables 24 we list YSO sources identified as Class I Class II and Class III in our region of study. P 3 data files.

2016-06-01T00:00:00Z

['10.26093/cds/vizier.51500191', '2016yCat..51500191R']

['YSOs', 'Photometry: infrared']

VizieR Online Data Catalog Infrared photometry of YSOs in CygnusX DR15 RiveraGalvez 2015

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2016yCat..74514346S

FLAMES observations towards four open clusters in the LMC and SMC were retrieved from the ESO archive and are used to study the IHVCs towards these galaxies and their variation on small scales. P 1 data file.

2016-06-01T00:00:00Z

['2016yCat..74514346S']

['Magellanic Clouds', 'Clusters: open']

VizieR Online Data Catalog Earlytype stars in SMC and LMC Smoker 2015

2016yCat..74512750X

Our sample was collected directly from the sample of Nemmen et al. 2012 Cat. JotherSci338.1445 but some blazars in Nemmen et al. 2012 Cat. JotherSci338.1445 were not clean Fermi blazars 2LAC Ackermann et al. 2011 Cat. JApJ743171. We removed the nonclean blazars. P 1 data file.

2016-01-01T00:00:00Z

['2016yCat..74512750X']

['BL Lac objects', 'QSOs', 'Gamma rays']

VizieR Online Data Catalog Blazar sequence Xiong 2015

2016wfc..rept....3D

We analyze 6 years of standard star observations acquired with the WFC3UVIS imager between 2009 and 2015. Observations of the three white dwarf standard stars GD 153 GD 71 and G191B2B were obtained at multiple dither positions near the center of the array and in all fourcorner subarrays. Departing from previous practice chipdependent inverse sensitivities are computed at r10 pixels 0.3962 arcsec for the 42 full frame filters excluding the 20 quad filters and these data also provide encircled energy fractions as a function of filter. Chipdependent inverse sensitivities differ on average by 3 from previous computations primarily due to drizzling errors. UVIS2 science data are scaled to UVIS1 by the inverse sensitivity ratio so that only a single photflam value is needed for the full detector. We describe the UVIS 2.0 chipdependent philosophy and discuss our results in the context of prior photometric calculations. An updated version of CALWF3 version 3.3 is required to process the new chipdependent solutions.

2016-11-01T00:00:00Z

['2016wfc..rept....3D']

['Hubble Space Telescope', 'HST', 'Space Telescope Science Institute', 'STScI', 'WFC3', 'UVIS', 'photometry', 'inverse sensitivity', 'two-chip']

UVIS 2.0 Chipdependent Inverse Sensitivity Values

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2016yCat..17810124C

A goal of this work is to find selfconsistent and accurate ways to predict the properties of stellar lightcurve variability and to use this variability to calibrate against other methods of determining their fundamental parameters. Thus it may be possible to develop the analysis of granular flicker measurements in a way that augments the results of asteroseismology and improves the accuracy of e.g. stellar mass and radius measurements. P To assist in this process we provide tabulated data for 508 stars with photometric light curves measured by the Kepler mission which also includes their derived masses and predicted values of the turbulent Mach number MSUBaSUB the rootmeansquare rms granulation intensity amplitude and the flicker amplitude FSUB8SUB. These data are also hosted with updates as needed on the first authors Web site httpwww.cfa.harvard.eduscranmer. With the data is a short code written in the Interactive Data Language IDL that reads the data and reproduces two of the three panels of Figure4 in the paper. P 3 data files.

2016-01-01T00:00:00Z

['10.26093/cds/vizier.17810124', '2016yCat..17810124C']

['Stars: double and multiple', 'Stars: masses', 'Effective temperatures']

VizieR Online Data Catalog Granulation model for 508 KIC stars Cranmer 2014

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2016yCat..35890110A

The data analysed in this publication comprise two distinct types of observations. The first is of SN II optical spectroscopy obtained during their photospheric phases i.e. from discovery to at most 100 days post explosion. These data are used to extract absorption line pEW measurements. The second data set is emission line spectral observations of host HII regions of SNe II. These are used to estimate SN II environment oxygen abundances which can be used as metallicity proxies. In the course of this work we compare our observational results with the predictions from the spectral models of Dessart et al. 2014MNRAS.440.1856D. P 2 data files.

2016-07-01T00:00:00Z

['2016yCat..35890110A', '10.26093/cds/vizier.35890110']

['H II regions', 'Supernovae']

VizieR Online Data Catalog SN II in host HII regions Anderson 2016

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2016xnnd.confE..18E

Galaxy clusters are located at the crossroads of intergalactic filaments and are still forming through the continuous merging and accretion of smaller structures from the surrounding cosmic web. Deep widefield Xray studies of the outskirts of the most massive clusters bring us valuable insight into the processes leading to the growth of cosmic structures. In addition cluster outskirts are privileged sites to search for the missing baryons which are thought to reside within the filaments of the cosmic web. I will present the XMM cluster outskirts project a VLP that aims at mapping the outskirts of 13 nearby clusters. Based on the results obtained with this program I will then explore ideas to exploit the capabilities of XMM during the next decade.

2016-06-01T00:00:00Z

['2016xnnd.confE..18E']

Cluster outskirts and the missing baryons

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2016yCat..35890078B

Individual time averaged spectra of HSUB2SUBSUP16SUP HSUB2SUBSUP18SUPO110101 lines observed with the Odin satellite as used for Fig. 1 map plus a partial map not shown in the paper Fig. 2 time evolution analysis and averages shown in Fig. 3. By default these are the averages of the two combinations of autocorrelatorreceiver tuned to the same frequency unless specified for the AOS spectrometer single receiver 555B2. IRAM 30m telescope spectra time averaged shown in Figs. 38 are also provided. Spectra obtained with the IRAM 30m telescope are 100 100kms extract from the wide band 200kHz sampling FTS spectra and the higher resolution 40kHz sampling VESPA autocorrelator for the HCSUP15SUPN line. One fits file per spectrum fits output from class httpwww.iram.frIRAMFRGILDAS. P object.dat Code Name Elem q e i H1 d AU deg mag C2012 F6 Lemmon 2456375.5 0.7312461 0.9985125 82.607966 7.96 C2013 R1 Lovejoy 2456651.5 0.8118182 0.9983297 64.040457 11.66 P 2 data files.

2016-03-01T00:00:00Z

['10.26093/cds/vizier.35890078', '2016yCat..35890078B']

['Comets', 'Radio lines', 'Spectra: millimetric/submm']

VizieR Online Data Catalog C2012 F6 Lemmon and C2013 R1 spectra Lovejoy Biver 2016

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2015AGUFMSH53A2479J

In this study we analyze the abundances of suprathermal heavy ions in 75 Corotating Interaction Region CIR events between January 1st 1995 and December 31st 2008. We correlate the heavy ion abundances in these CIRs with those measured in the solar wind and suprathermal populations upstream of these events. Our analysis reveals that the CIR suprathermal heavy ion abundances vary by nearly two orders of magnitude over the solar activity cycle with higher abundances e.g. FeO occurring during solar maximum and depleted values occurring during solar minimum. The abundances are also energy dependent with larger abundances at higher energies particularly during solar maximum. Following the method used by Mason et al. 2008 we correlate the CIR abundances with the corresponding solar wind and suprathermal values measured during 6hour intervals for upstream periods spanning 10 days prior to the start of each CIR event. This correlation reveals that suprathermal heavy ions are better correlated with upstream suprathermal abundances measured at the same energy compared with the solar wind heavy ion abundances. Using the 6hour averaging method we also identified timeframes of maximum correlation between the CIR and the upstream suprathermal abundances and find that the time of maximum correlation depends on the energy of the suprathermal ions. We discuss the implications of these results in terms of previous studies of CIR and suprathermal particles and CIR seed populations and acceleration mechanisms.

2015-12-01T00:00:00Z

['2015AGUFMSH53A2479J']

['2102 Corotating streams', 'INTERPLANETARY PHYSICS', '2126 Heliosphere/interstellar medium interactions', 'INTERPLANETARY PHYSICS', '7513 Coronal mass ejections', 'SOLAR PHYSICS', 'ASTROPHYSICS', 'AND ASTRONOMY', '7954 Magnetic storms', 'SPACE WEATHER']

Abundance and Source Population of Suprathermal Heavy Ions in Corotating Interaction Regions

2017GReGr..49...41K

It is shown that continuous causal isomorphisms on twodimensional Minkowski spacetime can be characterized by the invariance of wave equations.

2017-03-01T00:00:00Z

['2017GReGr..49...41K', '10.1007/s10714-017-2206-y']

['Causal isomorphism', 'Causal relation', 'Wave equation', "Zeeman's theorem"]

On continuous causal isomorphisms on twodimensional Minkowski spacetimes

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2017Ge&Ae..57..251B

An algorithm for retrieving the AL index dynamics from the parameters of solarwind plasma and the interplanetary magnetic field IMF has been developed. Along with other geoeffective parameters of the solar wind an integral parameter in the form of the cumulative sum NVSUP2SUP is used to determine the process of substorm formation. The algorithm is incorporated into a framework developed to retrieve the AL index of an Elmantype artificial neural network ANN containing an additional layer of neurons that provides an internal memory of the prehistory of the dynamical process to be retrieved. The ANN is trained on data of 70 eighthourlong time intervals including the periods of isolated magnetospheric substorms. The efficiency of this approach is demonstrated by numerical neuralnetwork experiments on retrieving the dynamics of the AL index from the of solar wind and IMF parameters during substorms.

2017-05-01T00:00:00Z

['10.1134/S0016793217030021', '2017Ge&Ae..57..251B']

Effect of solar dynamics parameters on the formation of substorm activity

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2017GCN.21929....1H

Our collaboration GROWTH JAGWAR CaltechNRAO TTUNRAO has continued to monitor the evolution of the radio counterpart to GW170817SSS17a discovered on September 23 2017 with the Jansky VLA Mooley et al. LVC GCN 21814 and Corsi et al. LVC GCN 21815 with ongoing observations at frequencies of 1.4 GHz 3 GHz and 6 GHz. Responding to a request for further information to help plan observations at other radio facilities we are including details on the most recent detection at 3 GHz wherein the source was detected at a flux density of 34 3.6 uJy on Sept 17 UT. The full light curves and interpretation have been submitted for publication Hallinan Corsi et al.. We thank the VLA staff for scheduling these observations.

2017-09-01T00:00:00Z

['2017GCN.21929....1H']

LIGOVIRGO G298048 Latest 3 GHz Detection of Radio Counterpart to SSS17a

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2017GCN.22122....1L

We have reanalysed offline noisesubtracted data for the LIGO Hanford Observatory H and the LIGO Livingston Observatory L around the time of the binary black hole merger event G288732 GW170608 GCNs 21221 and 21239 taking into account our most uptodate understanding of both calibration and waveform modelling uncertainties. Parameter estimation has been performed using LALInference Veitch et al. PRD 91 042003 and a new sky map LALInferenceP.fits.gz is available for retrieval from the GraceDB event page httpsgracedb.ligo.orgeventsG288732 The 50 and 90 credible regions span about 170 and 520 square degrees respectively. This is the preferred sky map at this time and the version that will appear in LVC 2017 GW170608 Observation of a 19solarmass binary black hole coalescence in preparation.

2017-11-01T00:00:00Z

['2017GCN.22122....1L']

LIGOVirgo G288732GW170608 updated localization from parameter estimation

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2017LPI....48.2103K

This work utilizes MNF technique to map the spectral variability and delineate various basaltic units. CSFD technique was used to determine the age of units.

2017-03-01T00:00:00Z

['2017LPI....48.2103K']

Volcanic and Compositional History of Mare Nectaris Using Chandrayaan1 Moon Mineralogy MapperM3 Data

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2017LPI....48.2205B

Participants in NASA Goddards Planetary Science Winter School design a flight instrument under consideration for proposal. We present results and future plans.

2017-03-01T00:00:00Z

['2017LPI....48.2205B']

Training Early Career Scientists in Flight Instrument Design Through Experiential Learning NASA Goddards Planetary Science Winter School

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2017LPI....48.1528M

We created a model to investigate the role of orbital variability on postNoachian martian climate and surface conditions.

2017-03-01T00:00:00Z

['2017LPI....48.1528M']

The Role of Obliquity in PostNoachian Martian Surface Conditions

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2017LPI....48.3002F

An introduction of imaging method of Lunar Regolith Penetrating Radar LRPR which will be carried by the CE5 lander.

2017-03-01T00:00:00Z

['2017LPI....48.3002F']

An Imaging Method of Change5 Lunar Regolith Penetrating Radar

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2017LPI....48.2304S

We perform coregistration of topographic data sets from orbital observations of the Moon to measure its rotational dynamics.

2017-03-01T00:00:00Z

['2017LPI....48.2304S']

Measurements of Moons Rotation by CoRegistration of Laser Altimeter Profiles and Stereo Terrain Models

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2017LPI....48.1904S

Fly me to the Moon Dark surfaces I shall find But colours I seek.

2017-03-01T00:00:00Z

['2017LPI....48.1904S']

Wavelengths Selection for LEDIlluminated Multispectral Imaging on PROSPECT for Luna27

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2017LPI....48.2799T

We expose the CM2 chondrite Murchison to a simulated micrometeorite impact event. Results include spectral data and nanoscale chemical and structural analyses.

2017-03-01T00:00:00Z

['2017LPI....48.2799T']

Analyzing the Chemical and Spectral Effects of Pulsed Laser Irradiation to Simulate Space Weathering of a Carbonaceous Chondrite

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2017LPI....48.2302J

Isotopes and volatile element estimates for a dry Moon are consistent with the recently proposed highenergy highangularmomentum giant impact model.

2017-03-01T00:00:00Z

['2017LPI....48.2302J']

Testing Models of Lunar Origin K Isotopes Radiogenic Isotopes and Volatile Elements

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