%...Journal: PASP
%...MainTag: '<UCP-HEADER'
%R=BibCode
%A=Authors
%B=Abstract
%c=Copyright
%D=Date of publication
%E=Electronic file
%F=Original File
%I=Institute and/or Footnotes
%J-last page
%K=Keywords
%M=Manuscript
%T=Title
%Z=Editor's Notes sup. meterial

%R 2005PASP..117....1D
%F ori/PASPv117n827 
%J-12
%M 205012
%DOI 10.1086/427790
%T High Proper Motion Stars. IV. Radial Velocities of 166 Luyten Half-Second
   Stars.
%A Dawson, P.C. (1)(2)
%I Department of Physics, Trent University, 1600 West Bank Drive, Peterborough,
   ON K9J 7B8, Canada; (pdawson@trentu.ca)
%A De Robertis, M.M. (1)(2)
%I Department of Physics and Astronomy, York University, 4700 Keele Street,
   Toronto, ON M3J 1P3, Canada
%B We present 178 radial velocity measurements for 166 late-type stars
   selected from the Luyten half-second (LHS) proper motion catalog. Space velocities
   are given for all but two of them. Most of the stars lie within 25 pc of
   the Sun, but the list includes a handful of high-velocity transients from
   the halo population. None of the derived space velocities is high enough,
   however, to provide any constraint on the escape speed at the solar circle.
   Twenty-six stars are discussed in somewhat more detail, and evidence is adduced
   that several of them may be velocity variables.
%K Stars: Kinematics
%K Stars: Late-Type
%I (1) Guest user, Canadian Astronomy Data Centre, which is operated by
   the Herzberg Institute of Astrophysics, National Research Council of Canada.
%I (2) Guest Investigator, Dominion Astrophysical Observatory, Herzberg
   Institute of Astrophysics, National Research Council of Canada

%R 2005PASP..117...13S
%F ori/PASPv117n827 
%J-21
%M 205004
%DOI 10.1086/427538
%T A Revised Geometry for the Magnetic Wind of {theta}^1^ Orionis C.
%A Smith, Myron A.
%I Catholic University of America, 3700 San Martin Drive, Baltimore, MD 21218;
   (msmith@stsci.edu)
%A Fullerton, Alex W. (1)
%I Department of Physics and Astronomy, University of Victoria, P.O. Box 3055,
   Victoria, BC V8W 3P6, Canada
%B The star {theta}^1^ Orionis C (O6-7 V) is often cited as a hot analog
   of Bp variables, because its optical and UV line and X-ray continuum fluxes
   modulate over the magnetic/rotational period. In this circumstance, one expects
   emission and absorption components of the UV resonance lines to vary as a
   flattened magnetosphere corotates with the star. In this paper, we reexamine
   the detailed velocity behavior of several strong UV lines. Whereas past work
   has focused on variations of the full profiles, we find that the blue and
   red wings of the C IV and N V resonance lines exhibit anticorrelated modulations.
   These appear as absorption excesses at large blueshifts and as flux elevations
   at moderate redshifts at the edge-on phase {phi}=0.5. No rest-frame absorption
   features, which are the typical signatures of cool, static disks surrounding
   Bp stars, can be detected at any phase. We suggest that this behavior is
   caused by two geometrically distinct components of the wind, which are defined
   by the relationship between the extent of a magnetic loop and the local Alfv\'en
   radius. Streams on field lines opening outside this radius are first channeled
   toward the magnetic equator, but after reaching the Alfven radius, they are
   forced outward by radiative forces, eventually to become an expanding radial
   outflow. This wind component causes blueshifted absorption as the corotating
   magnetic equatorial plane crosses the observer's line of sight ({phi}=0.5).
   The geometry of the inner component requires a more complicated interpretation.
   Wind streams first follow closed loops and collide at the magnetic equator
   with counterpart streams from the opposite pole. There they coalesce and
   fall back to the star along their original field lines. The high temperatures
   in these falling condensations cause the redshifted emission. The rapid circulation
   of these flows is likely the reason for the absence of signatures of a cool
   disk (e.g., zero-velocity absorptions at {phi}~0.5) in the strong UV lines.
%K Stars: Individual: Constellation Name: {theta}^1^ Orionis C
%K Stars: Activity
%K Stars: Circumstellar Matter
%K Stars: Magnetic Fields
%I (1) Current address: Department of Physics and Astronomy, The Johns Hopkins
   University, 3400 North Charles Street, Baltimore, MD 21218; (awf@pha.jhu.edu).

%R 2005PASP..117...22P
%F ori/PASPv117n827 
%J-31
%M 205005
%DOI 10.1086/427545
%T A CCD {\em BVI} Photometric Study of the Young, Highly Reddened Open Cluster
   NGC 6318.
%A Piatti, Andr\'es E.
%I Instituto de Astronom\'ia y F\'isica del Espacio, Casilla de Correo 67, Sucursal
   28, 1428 Buenos Aires, Argentina; (andres@iafe.uba.ar)
%A Clari\'a, Juan J.
%A Ahumada, Andrea V.
%I Observatorio Astron\'omico, Universidad Nacional de C\'ordoba, Laprida 854, 5000
   C\'ordoba, Argentina; (claria@mail.oac.uncor.edu), (andrea@mail.oac.uncor.edu)
%B We present CCD {\em BVI} photometry for the southern open cluster NGC
   6318. The sample consists of 9876 stars measured in an area of 13'.6x13'.6,
   extending down to V~21.5 mag. Star counts carried out within and outside
   the cluster region allowed us to estimate the cluster angular radius as ~8'.
   The comparison of the cluster color-magnitude diagrams with isochrones of
   the Geneva group yields E(B-V)=1.20+/-0.05, E(V-I)=1.55+/-0.10, and V-M_V_=15.45+/-0.35
   for logt=8.20 (t=160 Myr) and Z=0.020. NGC 6318 is then located at 2.1+/-0.5
   kpc from the Sun and 30 pc below the Galactic plane. Using the WEBDA open
   cluster database, we examined the structure of the Galactic disk along the
   line of sight of NGC 6318. Among the known clusters in this direction, HM
   1 and BH 222 are the farthest ones, while those located between 1 and 2 kpc
   of the Sun appear to be more absorbed than those expected to follow a quasi-linear
   extinction law.
%K Galaxy: Open Clusters and Associations: General
%K open clusters and associations: individual (NGC 6318)
%K Techniques: Photometric
%Z extended table

%R 2005PASP..117...32W
%F ori/PASPv117n827 
%J-36
%M 205001
%DOI 10.1086/427383
%T Thirteen-Color Photometry of Open Cluster M48.
%A Wu, Zhen-Yu
%A Zhou, Xu
%A Ma, Jun
%A Jiang, Zhao-Ji
%A Chen, Jian-Sheng
%I National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun
   Road, Beijing 100012, China; (zywu@bac.pku.edu.cn)
%B This paper presents 13 color CCD intermediate-band spectrophotometry
   of a field centered on the open cluster M48 (NGC 2548) from 400 to nearly
   1000 nm, taken with Beijing-Arizona-Taiwan-Connecticut (BATC) Color Survey
   photometric system. The fundamental parameters of this cluster are derived
   with a new method that is based on a comparison of the spectral energy distributions
   (SEDs) of cluster stars and the theoretical SEDs of Padova models. We find
   that the best-fitting age of M48 is 0.32 Gyr, with a distance of 780 pc,
   a reddening of E(B-V)=0.04, and a solar metallicity of Z=0.019.
%K Galaxy: Open Clusters and Associations: Individual: NGC Number: NGC 2548
%K Stars: General
%K Stars: Hertzsprung-Russell Diagram

%R 2005PASP..117...37S
%F ori/PASPv117n827 
%J-78
%M 205011
%DOI 10.1086/427737
%T Faint {\em BVRI} Photometric Sequences in Selected Fields.
%A Saha, A. (1)(2)
%A Dolphin, A.E. (1)(3)
%A Thim, F. (1)(4)
%I NOAO, P.O. Box 26732, Tucson, AZ 85726; (saha@noao.edu), (adolphin@as.arizona.edu),
   (thim@noao.edu)
%A Whitmore, B.
%I Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218;
   (whitmore@stsci.edu)
%B The results from work done to extend the Johnson-Cousins {\em BVRI}
   photometric standard sequence to faint levels of V~21 mag in compact fields
   is presented. Such calibration and extension of sequences is necessary to
   fill a calibration gap if reliable photometry from modest aperture telescopes
   in space (e.g., the {\em Hubble Space Telescope}) or terrestrial telescopes
   with apertures exceeding 4 m is to be done. Sequences like the ones presented
   here, which cover a large range in brightness as well as color, will allow
   photometric calibration to be done efficiently and will also make such work
   less prone to systematic sources of error. Photometry of stars in approximately
   10'x10' fields around three globular clusters (NGC 2419, Pal 4, and Pal
   14) are presented from data acquired over several photometric nights. In
   each field, several stars are measured in {\em B}, {\em V}, {\em R}, and
   {\em I} passbands, with standard errors in the mean less than 0.015 mag from
   random errors, to levels fainter than V=21 mag. It is shown that when tying
   to the Landolt standards on the Johnson-Cousins system, standard errors in
   the mean from systematic errors are typically well below 0.01 mag in all
   four bands (except for {\em B} in NGC 2419 and {\em R} in Pal 4), thus justifying
   the claim that these fields have been correctly calibrated. The primary context
   for the work presented here is that parts of these fields were observed repeatedly
   by the Wide Field Planetary Camera 2 (WFPC2) on the {\em HST}, and thus these
   newly calibrated sequences can be used to retroactively calibrate WFPC2 at
   various times over its operating life. In the past, WFPC2 data have had typical
   photometric zero-point uncertainties of a few hundredths of a magnitude,
   largely due to a lack of suitable standard stars. The sequences presented
   here have standard errors at the 0.01 mag level. They agree at the 0.02 mag
   level with other extant calibrations of the targets presented here, except
   in the {\em I} band, where there are color-dependent deviations of up to
   0.05 mag versus one other photometric sequence. There is no clear resolution
   of this difference: we present as much verification of the sequences presented
   here as possible. We argue that a very likely reason for such discrepancies
   is differences in the filter bandpass.:
%K Galaxy: Globular Clusters: Individual: NGC Number: NGC 2419
%K globular clusters: individual (Palomar 14)
%K Galaxy: Globular Clusters: Individual: Name: Palomar 4
%K Standards
%Z : FITS files, extended tables
%I (1) NOAO is operated by the Association of Universities for Research
   in Astronomy, Inc., (AURA) under cooperative agreement with the National
   Science Foundation.
%I (2) Sabbatical Visitor, Indian Institute of Astrophysics, Koramangala,
   Bangalore 560034, India.
%I (3) Current address: Steward Observatory, University of Arizona, 933
   North Cherry Avenue, Tucson, AZ 85721.
%I (4) Current address: Brandenburg GmbH, Technologiepark 19, 33100 Paderborn,
   Germany; (thim@brandenburg-gmbh.de).

%R 2005PASP..117...79W
%F ori/PASPv117n827 
%J-85
%M 205009
%DOI 10.1086/427710
%T Estimating Photometric Redshifts Using Support Vector Machines.
%A Wadadekar, Yogesh
%I Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218;
   (wadadekar@stsci.edu)
%B We present a new approach to obtaining photometric redshifts using a
   kernel learning technique called ``support vector machines.'' Unlike traditional
   spectral energy distribution fitting, this technique requires a large and
   representative training set. When one is available, however, it is likely
   to produce results that are comparable to the best results obtained using
   template fitting and artificial neural networks. Additional photometric parameters
   such as morphology, size, and surface brightness can be easily incorporated.
   The technique is demonstrated using samples of galaxies from the Sloan Digital
   Sky Survey Data Release 2 and the hybrid galaxy formation code GalICS. The
   rms error in redshift estimation is below 0.03 for both samples. The strengths
   and limitations of the technique are assessed.
%K Galaxies: Fundamental Parameters
%K Methods: Statistical

%R 2005PASP..117...86Z
%F ori/PASPv117n827 
%J-93
%M 205008
%DOI 10.1086/427735
%T Modeling the CCD Undersampling Effect in the BATC Photometric System.
%A Zhou, Xu (1)(2)
%A Sun, Wei-Hsin (2)
%A Jiang, Zhao-Ji (1)
%A Ma, Jun (1)
%A Zhang, Xiao-Bing (1)
%A Byun, Yong-Ik (3)
%A Chen, Wen-Ping (2)
%A Chen, Jian-Sheng (1)
%B In certain CCD imaging systems, ``intrapixel effects'' introduce nonnegligible
   errors into the photometric accuracy of these systems. This effect is presumably
   caused by undersampling of the point source image by individual CCD pixels. This
   undersampling effect shows that the exact location of the source image on
   a pixel determines the flux detected by that pixel. Thus, as the image center
   drifts, for various reasons, across a pixel in a series of exposures, a difference
   in the response from the center to the edge of a pixel results in a variation
   of flux readout by that pixel. This effect could be important under superb
   seeing conditions, mimicking microvariability in stellar photometry for imaging
   systems having certain plate scales. To study this effect in detail, we carried
   out a full-night monitoring of bright stars in a 14'x14' field using
   the Beijing-Arizona-Taipei-Connecticut (BATC) observing system. This 10 hr
   monitoring program shows that all the stars in the field vary periodically
   with almost the same amplitude and frequency, but that the variations were
   out of phase among the stars in the field. Furthermore, the variation of
   all the stars diminished toward the end of the night, as the seeing became
   worse. Since the flux variation correlates well with the precise location
   of the image center on a pixel, we attribute these phenomena to the ``intrapixel
   effect'' of our CCD imaging system. In this study, we describe the nature
   of this undersampling effect and its influence on the photometric accuracy.
   We found that this effect can be modeled and removed if the seeing conditions
   and the intrapixel positions and motions of stars on the CCD chip are known.
%K Instrumentation: Detectors
%K Techniques: Photometric
%K Methods: Data Analysis
%I (1) National Astronomical Observatories, Chinese Academy of Sciences,
   Beijing 100012, China; (zhouxu@bac.pku.edu.cn).
%I (2) Institute of Astronomy, National Central University, Chung-Li, Taiwan.
%I (3) Yonsei University Observatory, Seoul 120-749, Korea.

%R 2005PASP..117...94O
%F ori/PASPv117n827 
%J-103
%M 205006
%DOI 10.1086/427566
%T Memory-Efficient Up-the-Ramp Processing with Cosmic-Ray Rejection.
%A Offenberg, J.D. (1)(2)
%A Fixsen, D.J. (1)(2)
%A Mather, J.C. (2)
%B We introduce a memory-efficient method for processing up-the-ramp sampled
   data to reduce noise and remove cosmic-ray events. The method we describe
   includes initial processing in the readout electronics (onboard, in the case
   of a space mission) plus postprocessing downstream. This data processing
   approach can be used to record or downlink high-quality science data using
   a small fraction of the bits required to transmit the full data, potentially
   reducing the volume to 0.01-0.001 of its original size. The onboard component
   has the advantage that it ``processes as you go'', reducing the online memory
   requirements. The processing and memory requirements are modest and are within
   the scope of current-generation avionics systems. We discuss the requirements
   and the performance of the algorithm. We also demonstrate the quality of
   the resulting data.
%K Instrumentation: Detectors
%K Methods: Data Analysis
%K Methods: Miscellaneous
%K space vehicles: instruments
%K Techniques: Image Processing
%I (1) Science Systems and Applications, Inc., 10210 Greenbelt Road, Suite
   600, Lanham, MD 20706; (Joel.D.Offenberg.1@gsfc.nasa.gov).
%I (2) Laboratory for Astronomy and Solar Physics, NASA's Goddard Space
   Flight Center, Greenbelt, MD 20771.

%R 2005PASP..117..104C
%F ori/PASPv117n827 
%J-110
%M 205010
%DOI 10.1086/427736
%T High-Altitude Wind Velocity at Sierra Negra and San Pedro M\'artir.
%A Carrasco, Esperanza
%I Instituto Nacional de Astrof\'isica, \'Optica, y Electr\'onica, Luis Enrique Erro
   1, Tonantzintla, Puebla 72840, Mexico; (bec@inaoep.mx)
%A Avila, Remy (1)
%I Instituto de Astronom\'ia, UNAM, M\'exico D.F., Mexico; (r.avila@astrosmo.unam.mx)
%A Carrami\~nana, Alberto
%I Instituto Nacional de Astrof\'isica, \'Optica, y Electr\'onica, Luis Enrique Erro
   1, Tonantzintla, Puebla 72840, Mexico; (alberto@inaoep.mx)
%B It has been proposed that the global circulation of atmospheric winds
   at 200 mbar can be used as a criterion to establish the suitability of a
   site for the development of adaptive optics techniques such as slow wave
   front corrugation correction. By using the NOAA NCEP/NCAR reanalysis database,
   we analyze the monthly average wind velocity at 200 mbar for a 16 yr period
   for two sites in Mexico: Sierra Negra and San Pedro M\'artir. We compare the
   results with those obtained for Mauna Kea, Paranal, and La Silla, and with
   Maidanak in Uzbekistan and Gamsberg in Namibia. We show that for all the
   sites studied, there is a yearly wind speed modulation, and we model that
   modulation. Our results show that Sierra Negra and San Pedro M\'artir are comparable
   to the best observatory sites, such as Mauna Kea, and are among the best
   sites to apply adaptive optics techniques.
%K Site Testing
%K Atmospheric Effects
%I (1) On leave from Centro de Radioastronom\'ia y Astrof\'isica, UNAM, Morelia,
   Mexico.

%R 2005PASP..117..111T
%F ori/PASPv117n827 
%J-118
%M 205003
%DOI 10.1086/427460
%T Productivity and Impact of Optical Telescopes.
%A Trimble, Virginia
%A Zaich, Paul (1)
%A Bosler, Tammy (2)
%I Department of Physics and Astronomy, University of California, 4129 Frederick
   Reimes Hall, Irvine, CA 92697-4575; (vtrimble@uci.edu)
%B In 2001, about 2100 papers appearing in 18 journals reported and/or
   analyzed data collected with ground-based optical and infrared telescopes
   and the {\em Hubble Space Telescope}. About 250 telescopes were represented,
   including 25 with primary mirror diameters of 3 m or larger. The subjects
   covered in the papers divide reasonably cleanly into 20 areas, from solar
   system to cosmology. These papers were cited 24,354 times in 2002 and 2003,
   for a mean rate of 11.56 citations per paper, or 5.78 citations per paper
   per year (sometimes called impact or impact factor). We analyze here the
   distributions of the papers, citations, and impact factors among the telescopes
   and subject areas and compare the results with those of a very similar study
   of papers published in 1990-1991 and cited in 1993. Some of the results are
   exactly as expected. Big telescopes produce more papers and more citations
   per paper than small ones. There are fashionable topics (cosmology and exoplanets)
   and less fashionable ones (binary stars and planetary nebulae). And the {\em
   Hubble Space Telescope} has changed the landscape a great deal. Some other
   results surprised us but are explicable in retrospect. Small telescopes on
   well-supported sites (La Silla and Cerro Tololo, for instance) produce papers
   with larger impact factors than similar sized telescopes in relative isolation.
   Not just the fraction of all papers, but the absolute numbers of papers coming
   out of the most productive 4 m telescopes of a decade ago have gone down.
   The average number of citations per paper per year resulting from the 38
   telescopes (2 m and larger) considered in 1993 has gone up 38%, from 3.48
   to 4.81, a form, perhaps, of grade inflation. And 53% of the 2100 papers
   and 38% of the citations (including 44% of the papers and 31% of the citations
   from mirrors of 3 m and larger) pertain to topics often not regarded as major
   drivers for the next generation of still larger ground-based telescopes.
%K Telescopes
%K Sociology of Astronomy
%I (1) Current address: 5901 Sierra Bravo Road, Irvine, CA 92612.
%I (2) Current address: Hemauerstr 19B, Apartment 50, 93027 Regensburg,
   Germany.

%R 2005PASP..117..119G
%F ori/PASPv117n827 
%J-119
%M 205002
%DOI 10.1086/427384
%T Deviations from the Fundamental Plane of Early-Type Galaxies and Large-Scale
   Motions of Clusters. (Dissertation Summary).
%A Gibbons, Rachel A.
%I Current address: Vanderbilt University, Department of Physics and Astronomy,
   6301 Stevenson Center, Nashville, TN 37235-1807; (rachel.a.gibbons@vanderbilt.edu)Thesis
   work conducted at University of Maryland at College ParkPh.D. thesis directed
   by Andrew S. Fruchter; Ph.D. degree awarded 2002 August
%K Dissertation summary

%R 2005PASP..117..120P
%F ori/PASPv117n827 
%J-120
%M 205007
%DOI 10.1086/427632
%T The Star Formation Rate Density of the Universe at {\em z} = 0.24 and 0.4
   from H{alpha}. (Dissertation Summary).
%A Pascual, Sergio
%I Current address: Department of Astrophysics, Universidad Complutense de Madrid,
   E-28040, Madrid, Spain; (spr@astrax.fis.ucm.es)Thesis work conducted at Universidad
   Complutense de MadridPh.D. thesis directed by Jes\'us Gallego and Jaime Zamorano;
   Ph.D. degree awarded 2004 July 9
%K Dissertation summary