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Author name code: pavlenko
ADS astronomy entries on 2022-09-14
author:"Pavlenko, Yakov V." 

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Title: Bands of NaH lines in spectra of late type stars
Authors: Lyubchyk, Y. P.; Pavlenko, Y. V.; Lyubchyk, O. K.; Jones,
   H. R. A.
2022KFNT...38c..65L    Altcode:
  No abstract at ADS

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Title: Analysis of actinium abundances in the atmosphere of Cepheid
    HIP13962
Authors: Gopka, V. F.; Shavrina, A. V.; Yushchenko, V. A.; Pavlenko,
   Y. V.; Yushchenko, A. V.; Glazunova, L. V.
2022KFNT...38...63G    Altcode:
  No abstract at ADS

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Title: Exocomet activity around the stars at different evolution
stages: current issues
Authors: Pavlenko, Y. V.; Shubina, O. C.; Kulyk, I. V.; Kuznyetsova,
   Y. G.; Zakhozhay, O. V.; Korsun, P. P.; Borysenko, S. A.; Krushevska,
   V. M.; Andreev, M. V.
2021KFNT...37b..19P    Altcode: 2021KFNT...37...19P
  No abstract at ADS

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Title: VizieR Online Data Catalog: HARPS and X-shooter spectra of
    Southern M dwarfs (Kuznetsov+ 2019)
Authors: Kuznetsov, M. K.; Del Burgo, C.; Pavlenko, Y. V.; Frith, J.
2020yCat..18780134K    Altcode:
  The High-accuracy Radial-velocity Planet Searcher (HARPS) is a
  high-resolution spectrograph installed on the 3.6m telescope in La
  Silla. It has a resolving power of R~115000 over a spectral range of
  3830-6930Å. Using the ESO Science Archive Facility, we downloaded
  5567 spectra, obtained during a period between 2003 October and 2017
  February, which corresponded to 420 M dwarfs from our sample. <P />The
  X-shooter (Intermediate Resolution, High-Efficiency Spectrograph)
  spectrograph is mounted on the VLT at the European Southern Observatory
  (ESO) in Paranal, Chile. In this paper, we focused on data obtained from
  the VIS spectroscopic arm of the X-shooter (5340-10200Å). The available
  VIS spectra associated with the stars from our sample were retrieved
  from the European Southern Observatory (ESO) science archive. The
  spectra were observed between 2009 June and 2017 November. In total,
  we collected spectroscopic data for 153 stars. <P />(2 data files).

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Title: Isotopic ratios in the red giant component of the recurrent
    nova T Coronae Borealis
Authors: Pavlenko, Y. V.; Evans, A.; Banerjee, D. P. K.; Geballe,
   T. R.; Munari, U.; Gehrz, R. D.; Woodward, C. E.; Starrfield, S.
2020MNRAS.498.4853P    Altcode: 2020arXiv200812150P; 2020MNRAS.tmp.2568P
  We report the determination of abundances and isotopic ratios for C,
  O, and Si in the photosphere of the red giant (RG) component of the
  recurrent nova (RN) T Coronae Borealis from new 2.284-2.402 μm
  and 3.985-4.155 μm spectroscopy. Abundances and isotopic ratios
  in the photosphere may be affected by (i) processes in the RG
  interior which are brought to the surface during dredge-up and (ii)
  contamination of the RG, either during the common envelope phase of
  the binary evolution or by material synthesized in RN eruptions,
  or a combination of the two. We find that the abundances of C, O,
  and Si are reasonably consistent with the expected composition of
  an RG after first dredge-up, as is the <SUP>16</SUP>O/<SUP>17</SUP>O
  ratio. The <SUP>28</SUP>Si/<SUP>29</SUP>Si ratio is found to be 8.6 ±
  3.0, and that for <SUP>28</SUP>Si/<SUP>30</SUP>Si is 21.5 ± 3.0. The
  <SUP>12</SUP>C/<SUP>13</SUP>C ratio (10 ± 2) is somewhat lower than
  expected for first dredge-up. The <SUP>16</SUP>O/<SUP>18</SUP>O ratio
  (41 ± 3) is highly inconsistent with that expected either from RG
  evolution (~550) or from contamination of the RG by the products of
  a nova thermonuclear runaway. In particular, the C and O isotopic
  ratios taken in combination are a puzzle. We urge confirmation of
  our results using spectroscopy at high resolution. We also encourage
  a thorough theoretical study of the effects on the secondary star in
  an RN system of contamination by ejecta having anomalous abundances
  and isotopic ratios.

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Title: Erratum: The first planet detected in the WTS: an inflated
    hot-Jupiter in a 3.35 day orbit around a late F-star
Authors: Cappetta, M.; Saglia, R. P.; Birkby, J. L.; Koppenhoefer, J.;
   Pinfield, D. J.; Hodgkin, S. T.; Cruz, P.; Kovács, G.; Sipőcz, B.;
   Barrado, D.; Nefs, B.; Pavlenko, Y. V.; Fossati, L.; del Burgo, C.;
   Martín, E. L.; Snellen, I.; Barnes, J.; Campbell, D.; Catalan, S.;
   Gálvez-Ortiz, M. C.; Goulding, N.; Haswell, C.; Ivanyuk, O.; Jones,
   H.; Kuznetsov, M.; Lodieu, N.; Marocco, F.; Mislis, D.; Murgas, F.;
   Napiwotzki, R.; Palle, E.; Pollacco, D.; Sarro Baro, L.; Solano, E.;
   Steele, P.; Stoev, H.; Tata, R.; Zendejas, J.
2020MNRAS.497..916C    Altcode:
  No abstract at ADS

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Title: VizieR Online Data Catalog: Post-AGB candidates in LMC and
    SMC SALT spectra (Szczerba+, 2020)
Authors: Szczerba, R.; Hajduk, M.; Pavlenko; Ya. V.; Hrivnak, B. J.;
   Kaminsky; B. M.; Volk, K.; Siodmiak, N. Gezer I.; Zacs, L.; Pych,
   W.; Sarna, M.
2020yCat..36410142S    Altcode:
  Spectroscopic data from the South African Large Telescope shown on
  Figs. 2, 3 and 4 are available in fig2.dat, fig3.dat and fig4.dat,
  respectively. Each spectrum has 2 gaps: in the red setting (Figs.2
  and 3) 7130-7200Å and 8170-8220Å, in the blue setting (Fig.4)
  3550-3580Å and 3840-3850Å. In the notes to the tables description we
  use "the left part" of the spectrum for spectrum before the first gap,
  "the middle part" of the spectrum for spectrum between the two gaps,
  and "the right part" of the spectrum for spectrum above the second
  gap. <P />(4 data files).

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Title: HD 54361: evidence for the status of a low mass TP-AGB star
Authors: Začs, L.; Pukïtis, K.; Sperauskas, J.; Pavlenko, Y.;
   Schmidt, M.; Alksnis, O.
2020Ap&SS.365...27Z    Altcode:
  The mass of the cool carbon star HD 54361 was suspected to be high,
  assuming the membership in the stellar association CMa OB1, in
  conflict with the theory of stellar evolution. The Gaia parallax and
  a high-resolution spectrum in the wavelength region from about 4800
  to 6900 Å was employed in order to update the distance, atmospheric
  parameters and abundances using the method of spectral synthesis and
  new model atmospheres. Absorption lines are broad in the spectrum
  presumably because of a large macroturbulence, ξ<SUB>RT</SUB>=10
  ±1 kms-<SUP>1</SUP>. Radial-velocity monitoring revealed a scatter
  of about 4 km s<SUP>-1</SUP>, which reflects probably a large scale
  convection in the atmosphere. The effective temperature was found to
  be about 3200 K by modelling the wings of Na I D doublet, a somewhat
  higher than that estimated from the angular diameter. The difference
  in the temperature could be due to the light/colour variation. The
  abundances of iron peak elements calculated from less blended
  lines blueward of 5000 Å are near solar, [M/H]=0.0 ±0.2 dex. The
  neutron-capture elements are enhanced up to 1 dex. The parallax leads
  to the distance of 554<SUB>-41</SUB><SUP>+49</SUP>pc, the absolute
  magnitude, M<SUB>K</SUB>=-7.7 ±0.2 mag, and the bolometric magnitude,
  M<SUB>bol</SUB>(K )=-4.6 ±0.2 mag. The observed stellar parameters and
  abundances are typical values for the low mass ∼1.8 M<SUB>⊙</SUB>
  star on the TP-AGB branch according to the isochrone calculated for
  logAge (yr )=9.20 with solar initial metallicity. HD 54361 possibly
  belongs to the spike in the TP-AGB star numbers associated with the
  AGB-boosting effect.

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Title: Metallicity, temperature, and gravity scales of M subdwarfs
Authors: Lodieu, N.; Allard, F.; Rodrigo, C.; Pavlenko, Y.; Burgasser,
   A.; Lyubchik, Y.; Kaminsky, B.; Homeier, D.
2019A&A...628A..61L    Altcode: 2019arXiv190703674L
  <BR /> Aims: The aim of the project is to define
  metallicity/gravity/temperature scales for different spectral types of
  metal-poor M dwarfs. <BR /> Methods: We obtained intermediate-resolution
  ultraviolet (R ∼ 3300), optical (R ∼ 5400), and near-infrared (R
  ∼ 3900) spectra of 43 M subdwarfs (sdM), extreme subdwarfs (esdM),
  and ultra-subdwarfs (usdM) with the X-shooter spectrograph on the
  European Southern Observatory Very Large Telescope. We compared
  our atlas of spectra to the latest BT-Settl synthetic spectral
  energy distribution over a wide range of metallicities, gravities,
  and effective temperatures to infer the physical properties for
  the whole M dwarf sequence (M0-M9.5) at sub-solar metallicities
  and constrain the latest atmospheric models. <BR /> Results: The
  BT-Settl models accurately reproduce the observed spectra across the
  450-2500 nm wavelength range except for a few regions. We find that
  the best fits are obtained for gravities of log (g) = 5.0-5.5 for
  the three metal classes. We infer metallicities of [Fe/H] = -0.5,
  -1.5, and -2.0 ± 0.5 dex and effective temperatures of 3700-2600
  K, 3800-2900 K, and 3700-2900 K for subdwarfs, extreme subdwarfs,
  and ultra-subdwarfs, respectively. Metal-poor M dwarfs tend to be
  warmer by about 200 ± 100 K and exhibit higher gravity than their
  solar-metallicity counterparts. We derive abundances of several
  elements (Fe, Na, K, Ca, Ti) for our sample but cannot describe their
  atmospheres with a single metallicity parameter. Our metallicity
  scale expands the current scales available for mildly metal-poor
  planet-host low-mass stars. Our compendium of moderate-resolution
  spectra covering the 0.45-2.5 micron range represents an important
  resource for large-scale surveys and space missions to come. <P />All
  observed spectra are available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr/">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/628/A61">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/628/A61</A>Based
  on observations collected at the European Southern Observatory,
  Chile, under programmes 089.C-0140(A), 091.C-0264(A), 092.D-0600(A),
  and 093.C-0610(A).

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Title: VizieR Online Data Catalog: X-shooter spectra of 43 metal-poor
    M dwarfs (Lodieu+, 2019)
Authors: Lodieu, N.; Allard, F.; Rodrigo, C.; Pavlenko, Y.; Burgasser,
   A.; Lyubchik, Y.; Kaminsky, B.; Homeier, D.
2019yCat..36280061L    Altcode:
  We make public the ESO VLT X-shooter spectra of 43 subdwarfs spanning
  the 560-2500nm wavelength range. Each file contains wavelength (in
  nm) and the flux (in ergs/cm<SUP>2</SUP>/s/Angstroem) in the first
  and second column, respectively. Spectra are corrected for telluric
  absorption. Names of files are composed of spectral types of the source
  followed by the date of observations. <P />(2 data files).

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Title: SiO bands in infrared spectra of late spectral stars
Authors: Pavlenko, Y. V.
2019KFNT...35d..21P    Altcode:
  No abstract at ADS

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Title: Masses, oxygen, and carbon abundances in CHEPS dwarf stars
Authors: Pavlenko, Y. V.; Kaminsky, B. M.; Jenkins, J. S.; Ivanyuk,
   O. M.; Jones, H. R. A.; Lyubchik, Y. P.
2019A&A...621A.112P    Altcode: 2018arXiv181105011P
  Context. We report the results from the determination of stellar
  masses, carbon, and oxygen abundances in the atmospheres of 107
  stars from the Calan-Hertfordshire Extrasolar Planet Search (CHEPS)
  programme. Our stars are drawn from a population with a significantly
  super-solar metallicity. At least 10 of these stars are known to host
  orbiting planets. <BR /> Aims: In this work, we set out to understand
  the behaviour of carbon and oxygen abundance in stars with different
  spectral classes, metallicities, and V sin i within the metal-rich
  stellar population. <BR /> Methods: Masses of these stars were
  determined using data from Gaia DR2. Oxygen and carbon abundances
  were determined by fitting the absorption lines. We determined oxygen
  abundances with fits to the 6300.304 Å O I line, and we used 3 lines
  of the C I atom and 12 lines of the C<SUB>2</SUB> molecule for the
  determination of carbon abundances. <BR /> Results: We determine masses
  and abundances of 107 CHEPS stars. There is no evidence that the [C/O]
  ratio depends on V sin i or the mass of the star within our constrained
  range of masses, i.e. 0.82 &lt; M<SUB>*</SUB>/M<SUB>⊙</SUB> &lt;
  1.5 and metallicities - 0.27 &lt; [Fe/H] &lt; +0.39. We also confirm
  that metal-rich dwarf stars with planets are more carbon rich in
  comparison with non-planet host stars with a statistical significance
  of 96%. <BR /> Conclusions: We find tentative evidence that there
  is a slight offset to lower abundance and a greater dispersion in
  oxygen abundances relative to carbon. We interpret this as potentially
  arising because the production of oxygen is more effective at more
  metal-poor epochs. We also find evidence that for lower mass stars the
  angular momentum loss in stars with planets as measured by V sin i is
  steeper than stars without planets. In general, we find that the fast
  rotators (V sin i &gt; 5 km s<SUP>-1</SUP>) are massive stars. <P
  />Table A.3 is also available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/621/A112">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/621/A112</A>

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Title: Accuracies of abundance determinations in large spectroscopic
    surveys
Authors: Ivanyuk, Oleksiy; Pavlenko, Y. V.; Jenkins, J. S.; Jones,
   H. R. A.
2018gbx..confE..18I    Altcode:
  Along with our own results from the high resolution spectral analysis
  of the 107 metal rich F, G, K stars from the Calan-Hertfordshire
  Extrasolar Planet Search program (CHEPS) we discuss differences in
  the abundances of Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Ni, Cu, and Zn
  between a number of large spectroscopic surveys. Most authors tend to
  use stellar spectra to determine virtually all fundamental parameters
  including effective temperature and surface gravity. We attempted to
  recreate results for a dozen of common stars using available input
  parameters to highlight the real scale of errors this approach might
  induce. We confirm overabundance and light decline of α-elements versus
  metallicity in the metal-deficient domain from -0.4 to -0.2 dex. This
  trend changes for the metal-rich stars between 0.0 and 0.4 dex, but
  among α-elements only Na follows positive trend - along with Mn, Ni,
  Cu and Zn. Slight increase is also visible for Al. Ca continued to
  show a negative trend.

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Title: VizieR Online Data Catalog: Carbon and oxygen in 107 dwarf
    stars (Pavlenko+, 2019)
Authors: Pavlenko, Y. V.; Kaminsky, B. M.; Jenkins, J. S.; Ivanyuk,
   O. M.; Jones, H. R. A.; Lyubchik, Y. P.
2018yCat..36210112P    Altcode:
  We used the observed spectra obtained in the framework of the
  Calan-Hertfordshire Extrasolar Planet Search (CHEPS) programme (Jenkins
  et al., 2009ApJ...704..975J, Cat. J/ApJ/704/975). <P />All stars in
  our work were observed with the HARPS spectrograph (Mayor et al.,
  2003Msngr.114...20M) at a resolving power of 115,000, and since the
  spectra were taken as part of the CHEPS programme, whose primary goal
  is the detection of small planets orbiting these stars, the S/N of the
  spectra are all over 100 at a wavelength of 6000Å. The 107 stars in
  this work are primary targets for CHEPS. <P />Carbon and Oxygen in the
  CHEPS stars. Cases of the problematic determination of oxygen abundance
  due to the strong blending 6300.304Å OI line by telluric lines are
  marked by (*). The oxygen abundances determined by visual comparison
  of computed and observed spectra are marked by (+). <P />(1 data file).

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Title: The analysis of actinium abundance in the atmospheres of
    three Magellanic Clouds red supergiants stars
Authors: Gopka, V. F.; Shavrina, A. V.; Yushchenko, V. A.; Yushchenko,
   A. V.; Pavlenko, Y. V.; Andrievsky, S. M.; Vasileva, S. V.; Kim, C.;
   Jeong, Y.; Lyubchik, Y. P.
2018KFNT...34c..25G    Altcode:
  No abstract at ADS

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Title: Flare activity and photospheric analysis of Proxima Centauri
Authors: Pavlenko, Y.; Suárez Mascareño, A.; Rebolo, R.; Lodieu,
   N.; Béjar, V. J. S.; González Hernández, J. I.
2017A&A...606A..49P    Altcode: 2017arXiv170604678P
  Context. We present the analysis of emission lines in high-resolution
  optical spectra of the planet-host star Proxima Centauri (Proxima)
  classified as a M5.5V. <BR /> Aims: We carry out a detailed analysis
  of the observed spectra to get a better understanding of the physical
  conditions of the atmosphere of this star. <BR /> Methods: We identify
  the emission lines in a series of 147 high-resolution optical spectra
  of the star at different levels of activity and compare them with the
  synthetic spectra computed over a wide spectral range. <BR /> Results:
  Our synthetic spectra computed with the PHOENIX 2900/5.0/0.0 model
  atmosphere fits the observed spectral energy distribution from optical
  to near-infrared quite well. However, modelling strong atomic lines
  in the blue spectrum (3900-4200 Å) requires implementing additional
  opacity. We show that high-temperature layers in Proxima Centauri
  consist of at least three emitting parts: a) a stellar chromosphere
  where numerous emission lines form; we suggest that some emission cores
  of strong absorption lines of metals form there; b) flare regions above
  the chromosphere, where hydrogen Balmer lines up to high transition
  levels (10-2) form; and c) a stellar wind component with V<SUB>r</SUB> =
  -30 km s<SUP>-1</SUP> seen in some Balmer lines as blueshifted emission
  lines. We believe that the observed He line at 4026 Å in emission can
  be formed in that very hot region. <BR /> Conclusions: We show that the
  real structure of the atmosphere of Proxima is rather complicated. The
  photosphere of the star is best fit by a normal M5 dwarf spectrum. On
  the other hand, emission lines form in the chromosphere, flare regions,
  and extended hot envelope. <P />The movies are available at <A
  href="http://www.aanda.org/10.1051/0004-6361/201730733/olm">http://www.aanda.org</A>

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Title: VizieR Online Data Catalog: Spectroscopic properties for 107
    stars (Ivanyuk+, 2017)
Authors: Ivanyuk, O. M.; Jenkins, J. S.; Pavlenko, Y. V.; Jones,
   H. R. A.; Pinfield, D. J.
2017yCat..74684151I    Altcode:
  The tables contain derived stellar parameters and abundances along with
  the spectral ranges that we used for the line profile fitting. <P />(2
  data files).

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Title: New planetary systems from the Calan-Hertfordshire Extrasolar
    Planet Search
Authors: Jenkins, J. S.; Jones, H. R. A.; Tuomi, M.; Díaz, M.;
   Cordero, J. P.; Aguayo, A.; Pantoja, B.; Arriagada, P.; Mahu, R.;
   Brahm, R.; Rojo, P.; Soto, M. G.; Ivanyuk, O.; Becerra Yoma, N.;
   Day-Jones, A. C.; Ruiz, M. T.; Pavlenko, Y. V.; Barnes, J. R.; Murgas,
   F.; Pinfield, D. J.; Jones, M. I.; López-Morales, M.; Shectman, S.;
   Butler, R. P.; Minniti, D.
2017MNRAS.466..443J    Altcode: 2016arXiv160309391J
  We report the discovery of eight new giant planets, and updated orbits
  for four known planets, orbiting dwarf and subgiant stars using the
  CORALIE, HARPS, and MIKE instruments as part of the Calan-Hertfordshire
  Extrasolar Planet Search. The planets have masses in the range 1.1-5.4
  M<SUB>J</SUB>'s, orbital periods from 40 to 2900 d, and eccentricities
  from 0.0 to 0.6. They include a double-planet system orbiting the
  most massive star in our sample (HD147873), two eccentric giant
  planets (HD128356b and HD154672b), and a rare 14 Herculis analogue
  (HD224538b). We highlight some population correlations from the sample
  of radial velocity detected planets orbiting nearby stars, including
  the mass function exponential distribution, confirmation of the growing
  body of evidence that low-mass planets tend to be found orbiting more
  metal-poor stars than giant planets, and a possible period-metallicity
  correlation for planets with masses &gt;0.1 M<SUB>J</SUB>, based on a
  metallicity difference of 0.16 dex between the population of planets
  with orbital periods less than 100 d and those with orbital periods
  greater than 100 d.

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Title: Determination of abundances in atmospheres of F-, G-, K-dwarfs
Authors: Pavlenko, Y. V.
2017KFNT...33v..24P    Altcode:
  No abstract at ADS

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Title: Acne at The Bottom Of The Main Sequence
Authors: Barnes, John; Haswell, C.; Jenkins, J.; Jeffers, S.; Jones,
   H. R. A.; Lohr, M.; Pavlenko, Y.
2016csss.confE..10B    Altcode:
  Starspots are an important manifestation of stellar activity and
  yet their distribution patterns on the lowest mass stars is not well
  known. Time series spectra of fully convective M dwarfs taken in the
  red-optical with UVES reveal numerous line profile distortions which are
  interpreted as starspots. We derive Doppler images for four M4.5V - M9V
  stars and find that contrast ratios corresponding to photosphere-spot
  temperature differences of only 200-300 K are sufficient to model
  the timeseries spectra. Although more starspot structure is found
  at high latitudes, spots are reconstructed at a range of phases and
  latitudes with mean spot filling factors of only a few per cent. The
  occurrence of low-contrast spots at predominantly high latitudes is
  in general likely to be responsible for the low amplitude photometric
  variability seen in late-M dwarfs. The recovered starspot patterns
  are used to assess their effect on precision radial velocity surveys
  aimed at detecting planets around this population of stars.

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Title: VLT X-Shooter spectroscopy of the nearest brown dwarf binary
Authors: Lodieu, N.; Zapatero Osorio, M. R.; Rebolo, R.; Béjar,
   V. J. S.; Pavlenko, Y.; Pérez-Garrido, A.
2015A&A...581A..73L    Altcode: 2015arXiv150608848L
  <BR /> Aims: The aim of the project is to characterise the
  two components of the brown dwarf system nearest to the Sun,
  WISE J104915.57-531906.1 (also called Luhman 16AB) at optical
  and near-infrared wavelengths. <BR /> Methods: We obtained high
  signal-to-noise intermediate-resolution (R ~ 6000-11 000) optical
  (600-1000 nm) and near-infrared (1000-2480 nm) spectra of each
  component of Luhman 16AB with the X-Shooter instrument on the
  Very Large Telescope. <BR /> Results: We classify the primary and
  secondary of the Luhman 16 system as L6-L7.5 and T0±1, respectively,
  in agreement with previous measurements published in the literature. We
  present measurements of the lithium pseudo-equivalent widths, which
  appear of similar strength in both components (8.2 ± 1.0 Å for the
  L and 8.4 ± 1.5 Å for the T component). The presence of lithium
  (<SUP>7</SUP>Li) in both components implies masses lower than 0.06
  M<SUB>⊙</SUB>, while the comparison with models suggests lower
  limits of 0.04 M<SUB>⊙</SUB>. The detection of lithium in the T
  component is the first of its kind. Similarly, we assess the strength
  of other alkali lines (e.g. pseudo-equivalent widths of 6-7 Å for
  RbI and 4-7 Å for CsI) present in the optical and near-infrared
  regions and compare with estimates for L and T dwarfs. We also
  derive effective temperatures and luminosities of each component of
  the binary: -4.66 ± 0.08 dex and 1305 K for the L dwarf and -4.68
  ± 0.13 dex and 1320 K for the T dwarf. According to our radial
  velocity determinations, the binary does not appear to belong to any
  of the well-known moving group. Our preliminary theoretical analysis
  of the optical and J-band spectra indicates that the L- and T-type
  spectra can be reproduced with a single temperature and gravity but
  different relative chemical abundances, which strongly affects the
  spectral energy distribution of L/T transition objects. <P />Based on
  observations collected at the European Southern Observatory, Chile,
  under DDT programme 290.C-5200(B) (PI Lodieu).FITS files of the
  reduced spectra are only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/581/A73">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/581/A73</A>

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Title: VizieR Online Data Catalog: Luhman 16AB X-shooter spectra
    (Lodieu+, 2015)
Authors: Lodieu, N.; Zapatero Osorio, M. R.; Rebolo, R.; Bejar,
   V. J. S.; Pavlenko, Y.; Perez-Garrido, A.
2015yCat..35810073L    Altcode:
  VLT X-shooter optical and near-infrared spectra of each component of
  the nearest brown dwarf binary system Luhman 16AB are made public. The
  spectra cover the ~670nm to ~2480nm with a resolution of 11000 in the
  optical (670-1000nm) and 6200 in the near-infrared (1000-2480nm). Note:
  We observe a peak and a dip around 2080-2090nm in the spectra of the
  components of the system not seen in other T dwarfs, as a potential
  artefact in our X-shooter data. No other strong artefact is present
  in our data. <P />(2 data files).

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Title: VizieR Online Data Catalog: Ji light curves of WTS-2 (Birkby+,
    2014)
Authors: Birkby, J. L.; Cappetta, M.; Cruz, P.; Koppenhoefer,
   J.; Ivanyuk, O.; Mustill, A. J.; Hodgkin, S. T.; Pinfield, D. J.;
   Sipocz, B.; Kovacs, G.; Saglia, R.; Pavlenko, Y.; Barrado, D.; Bayo,
   A.; Campbell, D.; Catalan, S.; Fossati, L.; Galvez-Ortiz, M. -C.;
   Kenworthy, M.; Lillo-Box, J.; Martin, E. L.; Mislis, D.; de Mooij,
   E. J. W.; Nefs, S. V.; Snellen, I. A. G.; Stoev, H.; Zendejas, J.;
   Del Burgo, C.; Barnes, J.; Goulding, N.; Haswell, C. A.; Kuznetsov,
   M.; Lodieu, N.; Murgas, F.; Palle, E.; Solano, E.; Steele, P.; Tata, R.
2015yCat..74401470B    Altcode:
  The infrared light curves of the WTS were generated from time series
  photometry taken with the WFCAM imager mounted at the prime focus of
  UKIRT. <P />In order to confirm the transit of WTS-2 b and to help
  constrain the transit model, on 2010 July 18 we obtained further time
  series photometry in the Sloan i band using the Wide Field Camera (WFC)
  on the 2.5m Isaac Newton Telescope (INT) at Roque de Los Muchachos,
  La Palma. <P />(2 data files).

---------------------------------------------------------
Title: A search for lithium in metal-poor L dwarfs
Authors: Lodieu, N.; Burgasser, A. J.; Pavlenko, Y.; Rebolo, R.
2015A&A...579A..58L    Altcode: 2015arXiv150506858L
  <BR /> Aims: The aim of the project is to search for lithium in
  absorption at 6707.8 Å to constrain the nature and mass of the
  brightest low-metallicity L-type dwarfs (referred to as L subdwarfs)
  identified in large-scale surveys. <BR /> Methods: We obtained low- to
  intermediate-resolution (R ~ 2500-9000) optical (~560-770 nm) spectra
  of two mid-L subdwarfs, SDSS J125637.13-022452.4 (SDSS1256; sdL3.5)
  and 2MASS J162620.14+392519.5 (2MASS1626; sdL4) with spectrographs on
  the European Southern Observatory Very Large Telescope and the Gran
  Telescopio de Canarias. <BR /> Results: We report the presence of a
  feature at the nominal position of the lithium absorption doublet at
  6707.8 Å in the spectrum of SDSS1256, with an equivalent width of 66
  ± 27 Å at 2.4σ, which we identify as arising from a CaH molecular
  transition based on atmosphere models. We do not see any feature at
  the position of the lithium feature in the spectrum of 2MASS1626. The
  existence of overlapping molecular absorption sets a confusion detection
  limit of [Li/H] = -3 for equivalently typed L subdwarfs. We provided
  improved radial velocity measurements of -126±10 km s<SUP>-1</SUP> and
  -239±12 km s<SUP>-1</SUP> for SDSS1256 and 2MASS1626, respectively,
  as well as revised Galactic orbits. We implemented adjusting factors
  for the CaH molecule in combination with the NextGen atmosphere
  models to fit the optical spectrum of SDSS1256 in the 6200-7300 Å
  range. We also estimate the expected Li abundance from interstellar
  accretion ([Li/H] = -5), place limits on circumstellar accretion
  (10<SUP>9</SUP> g/yr), and discuss the prospects of Li searches
  in cooler L and T subdwarfs. <P />Optical spectra of SDSS1256 and
  2MASS 1626 are only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/579/A58">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/579/A58</A>Based
  on observations collected at the European Southern Observatory, Chile,
  under programmes 089.C-0883 and 091.C-0594A.Based on observations
  made with the Gran Telescopio Canarias (GTC), installed in the
  Spanish Observatorio del Roque de los Muchachos of the Instituto
  de Astrofísica de Canarias, in the island of La Palma (programmes
  GTC64_10B and GTC38_11A).

---------------------------------------------------------
Title: VizieR Online Data Catalog: Spectra of two mid-L subdwarfs
    (Lodieu+, 2015)
Authors: Lodieu, N.; Burgasser, A. J.; Pavlenko, Y.; Rebolo, R.
2015yCat..35790058L    Altcode:
  Intermediate-resolution optical spectra of SDSS J125637.13-022452.4 and
  2MASS J162620.14+392519.5 are provided. They have been obtained with
  FORS2 on the ESO Very Large Telescope (grism GRIS1200R+93) and OSIRIS
  on the Gran Telescopio de Canarias (grating R2500R), respectively. <P
  />(2 data files).

---------------------------------------------------------
Title: Silicate Dust in RS Ophiuchi
Authors: Rushton, M. T.; Woodward, C. E.; Helton, L. A.; Gehrz, R. D.;
   Evans, A.; Kaminsky, B.; Pavlenko, Y. V.; Eyres, S. P. S.; Maxwell, M.
2014ASPC..490..249R    Altcode:
  We present Spitzer IRS spectra of the recurrent nova RS Ophiuchi
  obtained between 2006 and 2009. The data show emission lines due to HI,
  [Ne II], [Ne V], [Ne VI] and [O IV] and the well known silicate features
  at 10 μm and 18 μm, whose behaviour are reported here. The silicate
  features are variable in the period covered by the observations,
  appearing strongest in our 2007 data. Interestingly, the central
  wavelength of the 18 μm band is shorter than observed in other
  symbiotic systems and other circumstellar environments, suggesting
  unusual grain properties in RS Oph. We report changes that have taken
  place in the dusty environment in RS Oph and investigate the properties
  of the dust grains.

---------------------------------------------------------
Title: Erratum: The first planet detected in the WTS: an inflated
    hot-Jupiter in a 3.35 d orbit around a late F star
Authors: Cappetta, M.; Saglia, R. P.; Birkby, J. L.; Koppenhoefer, J.;
   Pinfield, D. J.; Hodgkin, S. T.; Cruz, P.; Kovács, G.; Sipőcz, B.;
   Barrado, D.; Nefs, B.; Pavlenko, Y. V.; Fossati, L.; del Burgo, C.;
   Martín, E. L.; Snellen, I.; Barnes, J.; Campbell, D.; Catalan, S.;
   Gálvez-Ortiz, M. C.; Goulding, N.; Haswell, C.; Ivanyuk, O.; Jones,
   H.; Kuznetsov, M.; Lodieu, N.; Marocco, F.; Mislis, D.; Murgas, F.;
   Napiwotzki, R.; Palle, E.; Pollacco, D.; Sarro Baro, L.; Solano, E.;
   Steele, P.; Stoev, H.; Tata, R.; Zendejas, J.
2014MNRAS.444.3150C    Altcode: 2014arXiv1410.3235C
  We report the discovery of WTS-1b, the first extrasolar planet found
  by the WFCAM Transit Survey, which began observations at the 3.8-m
  United Kingdom Infrared Telescope (UKIRT) in August 2007. Light
  curves comprising almost 1200 epochs with a photometric precision of
  better than 1 per cent to J ~ 16 were constructed for ~60000 stars and
  searched for periodic transit signals. For one of the most promising
  transiting candidates, high-resolution spectra taken at the Hobby-Eberly
  Telescope (HET) allowed us to estimate the spectroscopic parameters of
  the host star, a late-F main sequence dwarf (V=16.13) with possibly
  slightly subsolar metallicity, and to measure its radial velocity
  variations. The combined analysis of the light curves and spectroscopic
  data resulted in an orbital period of the substellar companion of 3.35
  days, a planetary mass of 4.01 +- 0.35 Mj and a planetary radius of
  1.49+0.16-0.18 Rj. WTS-1b has one of the largest radius anomalies among
  the known hot Jupiters in the mass range 3-5 Mj. The high irradiation
  from the host star ranks the planet in the pM class.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Catalogue of bright (K&lt;9)
    M dwarfs (Frith+, 2013)
Authors: Frith, J.; Pinfield, D. J.; Jones, H. R. A.; Barnes, J. R.;
   Pavlenko, Y.; Martin, E. L.; Brown, C.; Kuznetsov, M. K.; Marocco,
   F.; Tata, R.; Cappetta, M.
2014yCat..74352161F    Altcode:
  Using the Position and Proper Motion Extended-L (PPMXL) catalogue,
  we have used optical and near-infrared colour cuts together with
  a reduced proper motion cut to find bright M dwarfs for future
  exoplanet transit studies. PPMXL's low proper motion uncertainties
  allow us to probe down to smaller proper motions than previous similar
  studies. We have combined unique objects found with this method to
  that of previous work to produce 8479 K&lt;9 M dwarfs. Low-resolution
  spectroscopy was obtained of a sample of the objects found using this
  selection method to gain statistics on their spectral type and physical
  properties. Results show a spectral-type range of K7-M4V. This catalogue
  is the most complete collection of K&lt;9 M dwarfs currently available
  and is made available here. <P />(1 data file).

---------------------------------------------------------
Title: WTS-2 b: a hot Jupiter orbiting near its tidal destruction
    radius around a K dwarf
Authors: Birkby, J. L.; Cappetta, M.; Cruz, P.; Koppenhoefer,
   J.; Ivanyuk, O.; Mustill, A. J.; Hodgkin, S. T.; Pinfield, D. J.;
   Sipőcz, B.; Kovács, G.; Saglia, R.; Pavlenko, Y.; Barrado, D.; Bayo,
   A.; Campbell, D.; Catalan, S.; Fossati, L.; Gálvez-Ortiz, M. -C.;
   Kenworthy, M.; Lillo-Box, J.; Martín, E. L.; Mislis, D.; de Mooij,
   E. J. W.; Nefs, S. V.; Snellen, I. A. G.; Stoev, H.; Zendejas, J.;
   del Burgo, C.; Barnes, J.; Goulding, N.; Haswell, C. A.; Kuznetsov,
   M.; Lodieu, N.; Murgas, F.; Palle, E.; Solano, E.; Steele, P.; Tata, R.
2014MNRAS.440.1470B    Altcode: 2014MNRAS.tmp..557B; 2014arXiv1402.5416B
  We report the discovery of WTS-2 b, an unusually close-in 1.02-d
  hot Jupiter (M<SUB>P</SUB> = 1.12M<SUB>J</SUB>, R<SUB>P</SUB>
  = 1.30R<SUB>J</SUB>) orbiting a K2V star, which has a possible
  gravitationally bound M-dwarf companion at 0.6 arcsec separation
  contributing ∼20 per cent of the total flux in the observed J-band
  light curve. The planet is only 1.5 times the separation from its
  host star at which it would be destroyed by Roche lobe overflow,
  and has a predicted remaining lifetime of just ∼40 Myr, assuming a
  tidal dissipation quality factor of Q_{*}^'}=10<SUP>6</SUP>. Q_{*}^'}
  is a key factor in determining how frictional processes within a host
  star affect the orbital evolution of its companion giant planets,
  but it is currently poorly constrained by observations. We calculate
  that the orbital decay of WTS-2 b would correspond to a shift in
  its transit arrival time of T<SUB>shift</SUB> ∼ 17 s after 15 yr
  assuming Q_{*}^'}=10<SUP>6</SUP>. A shift less than this would place a
  direct observational constraint on the lower limit of Q_{*}^'} in this
  system. We also report a correction to the previously published expected
  T<SUB>shift</SUB> for WASP-18 b, finding that T<SUB>shift</SUB> = 356
  s after 10 yr for Q_{*}^'}=10<SUP>6</SUP>, which is much larger than
  the estimated 28 s quoted in WASP-18 b discovery paper. We attempted
  to constrain Q_{*}^'} via a study of the entire population of known
  transiting hot Jupiters, but our results were inconclusive, requiring
  a more detailed treatment of transit survey sensitivities at long
  periods. We conclude that the most informative and straightforward
  constraints on Q_{*}^'} will be obtained by direct observational
  measurements of the shift in transit arrival times in individual
  hot Jupiter systems. We show that this is achievable across the mass
  spectrum of exoplanet host stars within a decade, and will directly
  probe the effects of stellar interior structure on tidal dissipation.

---------------------------------------------------------
Title: Abundances in the atmosphere, effective temperature and
    surface gravity of the subdwarf metal-poor star G 224-58 A
Authors: Kushniruk, I.; Pavlenko, Y. V.
2014ysc..conf...18K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A catalogue of bright (K &lt; 9) M dwarfs
Authors: Frith, J.; Pinfield, D. J.; Jones, H. R. A.; Barnes, J. R.;
   Pavlenko, Y.; Martin, E. L.; Brown, C.; Kuznetsov, M. K.; Marocco,
   F.; Tata, R.; Cappetta, M.
2013MNRAS.435.2161F    Altcode: 2013MNRAS.tmp.2106F; 2013arXiv1308.0501F
  Using the Position and Proper Motion Extended-L (PPMXL) catalogue,
  we have used optical and near-infrared colour cuts together with a
  reduced proper motion cut to find bright M dwarfs for future exoplanet
  transit studies. PPMXL's low proper motion uncertainties allow us to
  probe down to smaller proper motions than previous similar studies. We
  have combined unique objects found with this method to that of previous
  work to produce 8479 K &lt; 9 M dwarfs. Low-resolution spectroscopy was
  obtained of a sample of the objects found using this selection method to
  gain statistics on their spectral type and physical properties. Results
  show a spectral-type range of K7-M4V. This catalogue is the most
  complete collection of K &lt; 9 M dwarfs currently available and is
  made available here.

---------------------------------------------------------
Title: A hot Jupiter transiting a mid-K dwarf found in the
    pre-OmegaCam Transit Survey
Authors: Koppenhoefer, J.; Saglia, R. P.; Fossati, L.; Lyubchik,
   Y.; Mugrauer, M.; Bender, R.; Lee, C. -H.; Riffeser, A.; Afonso,
   P.; Greiner, J.; Henning, Th.; Neuhäuser, R.; Snellen, I. A. G.;
   Pavlenko, Y.; Verdugo, M.; Vogt, N.
2013MNRAS.435.3133K    Altcode: 2013MNRAS.tmp.2185K; 2013arXiv1308.6574K
  We describe the pre-OmegaTranS project, a deep survey for transiting
  extra-solar planets in the Carina region of the Galactic disc. In
  2006-2008, we observed a single dense stellar field with a very high
  cadence of ∼2 min using the European Southern Observatory Wide
  Field Imager at the La Silla Observatory. <P />Using the Astronomical
  Wide-field Imaging System for Europe environment and the Munich
  Difference Imaging Analysis pipeline, a module that has been developed
  for this project, we created the light curves of 16 000 stars with more
  than 4000 data points which we searched for periodic transit signals
  using a box-fitting least-squares detection algorithm. All light curves
  are publicly available. In the course of the pre-OmegaTranS project,
  we identified two planet candidates - POTS-1b and POTS-C2b - which we
  present in this work. <P />With extensive follow-up observations we
  were able to confirm one of them, POTS-1b, a hot Jupiter transiting a
  mid-K dwarf. The planet has a mass of 2.31 ± 0.77 M<SUB>Jup</SUB>,
  a radius of 0.94 ± 0.04 R<SUB>Jup</SUB> and a period of P = 3.16
  d. The host star POTS-1 has a radius of 0.59 ± 0.02 R<SUB>⊙</SUB>
  and a mass of 0.70 ± 0.05 M<SUB>⊙</SUB>. Due to its low apparent
  brightness of I = 16.1 mag, the follow-up and confirmation of POTS-1b
  was particularly challenging and costly.

---------------------------------------------------------
Title: A Hot Uranus Orbiting the Super Metal-rich Star HD 77338 and
    the Metallicity-Mass Connection
Authors: Jenkins, J. S.; Jones, H. R. A.; Tuomi, M.; Murgas, F.; Hoyer,
   S.; Jones, M. I.; Barnes, J. R.; Pavlenko, Y. V.; Ivanyuk, O.; Rojo,
   P.; Jordán, A.; Day-Jones, A. C.; Ruiz, M. T.; Pinfield, D. J.
2013ApJ...766...67J    Altcode: 2012arXiv1207.1012J
  We announce the discovery of a low-mass planet orbiting the
  super metal-rich K0V star HD 77338 as part of our ongoing
  Calan-Hertfordshire Extrasolar Planet Search. The best-fit planet
  solution has an orbital period of 5.7361 ± 0.0015 days and with a
  radial velocity semi-amplitude of only 5.96 ± 1.74 ms<SUP>-1</SUP>,
  we find a minimum mass of 15.9^{+4.7}_{-5.3} M <SUB>⊕</SUB>. The
  best-fit eccentricity from this solution is 0.09^{+0.25}_{-0.09},
  and we find agreement for this data set using a Bayesian analysis
  and a periodogram analysis. We measure a metallicity for the star
  of +0.35 ± 0.06 dex, whereas another recent work finds +0.47 ±
  0.05 dex. Thus HD 77338b is one of the most metal-rich planet-host
  stars known and the most metal-rich star hosting a sub-Neptune-mass
  planet. We searched for a transit signature of HD 77338b but none was
  detected. We also highlight an emerging trend where metallicity and
  mass seem to correlate at very low masses, a discovery that would be
  in agreement with the core accretion model of planet formation. The
  trend appears to show that for Neptune-mass planets and below, higher
  masses are preferred when the host star is more metal-rich. Also a lower
  boundary is apparent in the super metal-rich regime where there are no
  very low mass planets yet discovered in comparison to the sub-solar
  metallicity regime. A Monte Carlo analysis shows that this low-mass
  planet desert is statistically significant with the current sample
  of 36 planets at the ~4.5σ level. In addition, results from Kepler
  strengthen the claim for this paucity of the lowest-mass planets in
  super metal-rich systems. Finally, this discovery adds to the growing
  population of low-mass planets around low-mass and metal-rich stars and
  shows that very low mass planets can now be discovered with a relatively
  small number of data points using stable instrumentation. <P />Based
  on observations collected at the La Silla Paranal Observatory, ESO
  (Chile) with the HARPS spectrograph on the ESO 3.6 m telescope, under
  the program IDs 079.C-0927, 081.C-0148, 087.C-0368, and 088.C-0662.

---------------------------------------------------------
Title: WTS-2 b: Too close for comfort?
Authors: Birkby, J. L.; Cappetta, M.; Cruz, P.; Koppenhoefer, J.;
   Ivanyuk, O.; Mustill, A.; Hodgkin, S. T.; Pinfield, D. J.; Sipőcz,
   B.; Kovács, G.; Saglia, R.; Pavlenko, Y.; RoPACS Collaboration;
   del Burgo, Carlos
2013EPJWC..4701004B    Altcode:
  We report the discovery of WTS-2 b, a typical hot Jupiter in an
  unusually close 1.02-day orbit to a K-dwarf star. This is the second
  planet to be discovered in the infrared light curves of the WFCAM
  Transit Survey (WTS) and is only one-and-a-half times the separation
  from its host star at which is would be destroyed by Roche lobe
  overflow. The predicted remaining lifetime of the planet is just 38
  Myrs, assuming a tidal dissipation quality factor of Q'<SUB>*</SUB> =
  10<SUP>6</SUP>. The magnitude of Q'<SUB>*</SUB> is largely unconstrained
  by observations, thus WTS-2 b provides a useful calibration point for
  theories describing how frictional processes within a host star affect
  the tidal orbital evolution of its companion giant planets. It is
  expected that stars with large convective envelopes are more efficient
  at dissipating the orbital energy of the planet, and WTS-2 b provides an
  observational constraint in the sparsely populated K-dwarf regime. In
  addition, despite its relatively faint magnitude, the favourable size
  ratio of the WTS-2 star-planet system and the predicted hot equilibrium
  temperature of the planet will make it possible to characterise the
  planet's atmosphere via secondary eclipse measurements using existing
  ground-based instrumentation.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Detached M dwarf eclipsing binaries
    in WTS (Birkby+, 2012)
Authors: Birkby, J.; Nefs, B.; Hodgkin, S.; Kovacs, G.; Sipocz, B.;
   Pinfield, D.; Snellen, I.; Mislis, D.; Murgas, F.; Lodieu, N.; de
   Mooij, E.; Goulding, N.; Cruz, P.; Stoev, H.; Cappetta, M.; Palle,
   E.; Barrado, D.; Saglia, R.; Martin, E.; Pavlenko, Y.
2013yCat..74261507B    Altcode:
  We identified our new MEBs using observations from the WTS (WFCAM
  Transit Survey). The WTS is an ongoing photometric monitoring campaign
  that operates on the 3.8-m United Kingdom Infrared Telescope (UKIRT)
  at Mauna Kea, Hawaii. <P />The survey began on 2007 August 5, and the
  eclipsing systems presented in this paper are all found in just one of
  the four WTS fields. <P />Photometric follow-up observations to help
  test and refine our light-curve models were obtained in the Sloan i
  band using the Wide-Field Camera (WFC) on the 2.5-m INT at Roque de
  Los Muchachos, La Palma. <P />(6 data files).

---------------------------------------------------------
Title: The spectroscopic study of M8.5-M9.5 stars and brown dwarfs
Authors: Kuznetsov, M. K.; Pavlenko, Y. V.; Galvez-Ortiz, M. C.
2013EPJWC..4704002K    Altcode:
  We present high-resolution spectra analysis of the three late-M dwarfs
  LP944-20, SIPS J2045-6332 and DENIS-P J0021.0-4244. The stellar spectra
  were observed with Very Large Telescope/Ultraviolet-Visual Echelle
  Spectrograph (VLT/UVES) in optical and near-infrared regions. The
  effective temperatures T<SUB>eff</SUB> and log g was defined by
  comparing observed and theoretical energy distributions for the
  investigated objects. Synthetic spectra were calculated for PHOENIX
  atmosphere models - COND and DUSTY, as well as for Semi-empirical
  atmosphere model. We discuss the influence of the effects associated
  with dust in stellar atmosphere on the energy distribution in the
  stellar spectra.

---------------------------------------------------------
Title: The Abundances of Heavy Elements in Red Supergiants of
    Magellanic Clouds
Authors: Gopka, V.; Yushchenko, A.; Kovtyukh, V.; Shavrina, A.;
   Yushchenko, V.; Vasilyeva, S.; Pavlenko, Y.; Andrievsky, S.
2013OAP....26...54G    Altcode:
  The spectra of Magellanic Clouds (MC) supergiants PMMR23, PMMR144
  and RM 1-667 with resolving power R=30,000 and signal to noise ratio
  near 100 obtained at 3.6 meter telescope in Chile were analysed. We
  present are port on the detailed investigation of MC supergiants,
  with special attention to the thorium abundance in these stars. The
  abundance patterns of three supergiants show that r-process elements
  are clearly detected in the atmospheres of investigated stars, but
  the bundances of s-processes elements can vary from star to star.

---------------------------------------------------------
Title: The first planet detected in the WTS: an inflated hot Jupiter
    in a 3.35 d orbit around a late F star
Authors: Cappetta, M.; Saglia, R. P.; Birkby, J. L.; Koppenhoefer, J.;
   Pinfield, D. J.; Hodgkin, S. T.; Cruz, P.; Kovács, G.; Sipőcz, B.;
   Barrado, D.; Nefs, B.; Pavlenko, Y. V.; Fossati, L.; del Burgo, C.;
   Martín, E. L.; Snellen, I.; Barnes, J.; Bayo, A.; Campbell, D. A.;
   Catalan, S.; Gálvez-Ortiz, M. C.; Goulding, N.; Haswell, C.; Ivanyuk,
   O.; Jones, H. R.; Kuznetsov, M.; Lodieu, N.; Marocco, F.; Mislis, D.;
   Murgas, F.; Napiwotzki, R.; Palle, E.; Pollacco, D.; Sarro Baro, L.;
   Solano, E.; Steele, P.; Stoev, H.; Tata, R.; Zendejas, J.
2012MNRAS.427.1877C    Altcode: 2012arXiv1210.1217C
  We report the discovery of WTS-1b, the first extrasolar planet found
  by the WFCAM Transit Survey, which began observations at the 3.8-m
  United Kingdom Infrared Telescope (UKIRT) in 2007 August. Light
  curves comprising almost 1200 epochs with a photometric precision
  of better than 1 per cent to J ∼ 16 were constructed for ∼60 000
  stars and searched for periodic transit signals. For one of the most
  promising transiting candidates, high-resolution spectra taken at the
  Hobby-Eberly Telescope (HET) allowed us to estimate the spectroscopic
  parameters of the host star, a late-F main-sequence dwarf (V = 16.13)
  with possibly slightly subsolar metallicity, and to measure its radial
  velocity variations. The combined analysis of the light curves and
  spectroscopic data resulted in an orbital period of the substellar
  companion of 3.35 d, a planetary mass of 4.01 ± 0.35 M<SUB>J</SUB>
  and a planetary radius of 1.49-0.18+0.16 R<SUB>J</SUB>. WTS-1b has
  one of the largest radius anomalies among the known hot Jupiters in
  the mass range 3-5 M<SUB>J</SUB>. The high irradiation from the host
  star ranks the planet in the pM class. Based on observations collected
  at the 3.8-m United Kingdom Infrared Telescope (Hawaii, USA), the
  Hobby-Eberly Telescope (Texas, USA), the 2.5-m Isaac Newton Telescope
  (La Palma, Spain), the William Herschel Telescope (La Palma, Spain),
  the German-Spanish Astronomical Centre (Calar Alto, Spain), the Kitt
  Peak National Observatory (Arizona, USA) and the Hertfordshire's
  Bayfordbury Observatory.

---------------------------------------------------------
Title: Lithium abundance in atmospheres of F- and G-type supergiants
    and bright giants
Authors: Lyubimkov, Leonid S.; Lambert, David L.; Kaminsky, Bogdan M.;
   Pavlenko, Yakov V.; Poklad, Dmitry B.; Rachkovskaya, Tamara M.
2012MNRAS.427...11L    Altcode: 2012arXiv1212.6057L
  Lithium in the atmosphere of a F or G supergiant reflects the initial
  Li abundance and the internal history of the star. During evolution of a
  star from the main sequence (MS) to the supergiant phase, lithium may be
  destroyed by, for example, rotationally induced mixing in the MS stars
  and strongly diluted by development of the supergiant's convective
  envelope. In order to probe the connection between atmospheric
  Li abundance and evolutionary predictions, we present a non-local
  thermodynamic equilibrium abundance analysis of the resonance doublet
  Li I at 6707.8 Å for 55 Galactic F and G supergiants and bright
  giants (we observed 43 of them, the remaining 12 are added from Luck
  and Wepfer's list). The derived lithium abundances log ɛ(Li) may be
  considered in three groups, namely: (i) 10 Li-rich giants with log
  ɛ(Li) = 2.0-3.2 (all 10 are F-type or A9 stars); (ii) 13 G- to K0-type
  stars with Li abundances in the narrow range log ɛ(Li) = 1.1-1.8;
  (iii) all other stars provide just upper limits to the Li abundance. <P
  />The derived Li abundances are compared with theoretical predictions
  of 2-15 M<SUB>⊙</SUB> stars (both rotating and non-rotating). Our
  results are generally in good agreement with theory. In particular,
  the absence of detectable lithium for the majority of programme stars
  is explainable. The comparison suggests that the stars may be separated
  by mass M into two groups, namely M ≲ 6 M<SUB>⊙</SUB> and M &gt;
  6 M<SUB>⊙</SUB>. All Li-rich giants and supergiants with log ɛ(Li)
  ≥ 2.0 have masses M &lt; 6 M<SUB>⊙</SUB>; this conclusion follows
  not only from our work but also from a scrutiny of published data. 11 of
  13 stars with log ɛ(Li) = 1.1-1.8, specifically the stars with M &lt;
  6 M<SUB>⊙</SUB>, show good agreement with the post-first dredge-up
  surface abundance log ɛ(Li) ≈ 1.4 predicted for the non-rotating 2-6
  M<SUB>⊙</SUB> stellar models. An absence of Li-rich stars in the range
  M &gt; 6 M<SUB>⊙</SUB> agrees with the theoretical prediction that F
  and G supergiants and giants with M &gt; 6 M<SUB>⊙</SUB> cannot show
  detectable lithium. <P />We note that present theory appears unable to
  account for the derived Li abundances for some stars, namely for (i) a
  few relatively low-mass Li-rich giants (M &lt; 6 M<SUB>⊙</SUB>), whose
  high Li abundances accompanied by rather high rotational velocities
  or substantial nitrogen excess contradict theoretical predictions;
  (ii) the relatively high-mass supergiants HR 461 and HR 8313 (M &gt;
  6 M<SUB>⊙</SUB>) with the detected abundances log ɛ = 1.3-1.5. It
  is possible that the lithium in such stars was synthesized recently.

---------------------------------------------------------
Title: Intermediate Resolution Near-infrared Spectroscopy of 36 Late
    M Dwarfs
Authors: Deshpande, R.; Martín, E. L.; Montgomery, M. M.; Zapatero
   Osorio, M. R.; Rodler, F.; del Burgo, C.; Phan Bao, N.; Lyubchik,
   Y.; Tata, R.; Bouy, H.; Pavlenko, Y.
2012AJ....144...99D    Altcode: 2012arXiv1207.2781D
  We present observations of 36 late M dwarfs obtained with the Keck
  II/NIRSPEC in the J band at a resolution of ~20,000. We have measured
  projected rotational velocities, absolute radial velocities, and
  pseudo-equivalent widths of atomic lines. Twelve of our targets did not
  have previous measurements in the literature. For the other 24 targets,
  we confirm previously reported measurements. We find that 13 stars
  from our sample have v sin i below our measurement threshold (12 km
  s<SUP>-1</SUP>) whereas four of our targets are fast rotators (v sin i
  &gt; 30 km s<SUP>-1</SUP>). As fast rotation causes spectral features to
  be washed out, stars with low projected rotational velocities are sought
  for radial velocity surveys. At our intermediate spectral resolution,
  we have confirmed the identification of neutral atomic lines reported
  in McLean et al. We also calculated pseudo-equivalent widths of 12
  atomic lines. Our results confirm that the pseudo-equivalent width of
  K I lines is strongly dependent on spectral types. We observe that the
  pseudo-equivalent width of Fe I and Mn I lines remains fairly constant
  with later spectral type. We suggest that these lines are particularly
  suitable for deriving metallicities for late M dwarfs.

---------------------------------------------------------
Title: Four ultra-short-period eclipsing M-dwarf binaries in the
    WFCAM Transit Survey
Authors: Nefs, S. V.; Birkby, J. L.; Snellen, I. A. G.; Hodgkin, S. T.;
   Pinfield, D. J.; Sipőcz, B.; Kovacs, G.; Mislis, D.; Saglia, R. P.;
   Koppenhoefer, J.; Cruz, P.; Barrado, D.; Martin, E. L.; Goulding, N.;
   Stoev, H.; Zendejas, J.; del Burgo, C.; Cappetta, M.; Pavlenko, Y. V.
2012MNRAS.425..950N    Altcode: 2012MNRAS.tmp.3514N; 2012arXiv1206.1200N
  We report on the discovery of four ultra-short-period (P ≤ 0.18 d)
  eclipsing M-dwarf binaries in the Wide-Field Camera (WFCAM) Transit
  Survey. Their orbital periods are significantly shorter than that of
  any other known main-sequence binary system, and are all significantly
  below the sharp period cut-off at P ∼ 0.22 d as seen in binaries of
  earlier-type stars. The shortest-period binary consists of two M4-type
  stars in a P = 0.112 d orbit. The binaries are discovered as part of
  an extensive search for short-period eclipsing systems in over 260
  000 stellar light curves, including over 10 000 M-dwarfs down to J =
  18 mag, yielding 25 binaries with P ≤ 0.23 d. In a popular paradigm,
  the evolution of short-period binaries of cool main-sequence stars is
  driven by the loss of angular momentum through magnetized winds. In
  this scheme, the observed P ∼ 0.22 d period cut-off is explained as
  being due to time-scales that are too long for lower-mass binaries to
  decay into tighter orbits. Our discovery of low-mass binaries with
  significantly shorter orbits implies that either these time-scales
  have been overestimated for M-dwarfs, e.g. due to a higher effective
  magnetic activity, or the mechanism for forming these tight M-dwarf
  binaries is different from that of earlier-type main-sequence stars.

---------------------------------------------------------
Title: Coupled azimuthal modes propagating in current-carrying
    plasma waveguides
Authors: Girka, V.; Girka, I.; Pavlenko, I.; Girka, O.; Girka, A.
2012JPlPh..78..105G    Altcode:
  The paper is devoted to the theory of electromagnetic surface
  waves propagating along the azimuthal direction in cylindrical metal
  waveguides, which are filled with current-carrying plasmas. The problem
  is solved by the method of successive approximation. Adequacy of this
  method application is proved here. To study the coupling of ordinary
  (O-) and extraordinary (X-) azimuthal modes, the linear theory of the
  eigenazimuthal X- and O-modes is applied as zero approximation. Plasma
  particles are described in the framework of magneto-hydrodynamics,
  electromagnetic fields of the coupled azimuthal modes are determined
  from Maxwell equations. Spatial distribution of electromagnetic field
  of these coupled modes and their damping caused for different reasons
  are studied. Possibility to observe experimentally the phenomena,
  which accompany propagation of these coupled modes, is estimated
  numerically. Branches of their possible utilization are discussed
  as well.

---------------------------------------------------------
Title: Benchmark cool companions: ages and abundances for the PZ
    Telescopii system
Authors: Jenkins, J. S.; Pavlenko, Y. V.; Ivanyuk, O.; Gallardo,
   J.; Jones, M. I.; Day-Jones, A. C.; Jones, H. R. A.; Ruiz, M. T.;
   Pinfield, D. J.; Yakovina, L.
2012MNRAS.420.3587J    Altcode: 2011arXiv1111.7001J
  We present new ages and abundance measurements for the pre-main-sequence
  star PZ Telescopii (more commonly known as PZ Tel). PZ Tel was
  recently found to host a young and low-mass companion. Such
  companions, whether they are brown dwarfs or planetary systems,
  can attain benchmark status by detailed study of the properties of
  the primary, and then evolutionary and bulk characteristics can be
  inferred for the companion. Using Fibre-fed Extended Range Optical
  Spectrograph spectra, we have measured atomic abundances (e.g. Fe
  and Li) and chromospheric activity for PZ Tel and used these to
  obtain the metallicity and age estimates for the companion. We have
  also determined the age independently using the latest evolutionary
  models. We find PZ Tel A to be a rapidly rotating (v sin i= 73 ± 5
  km s<SUP>-1</SUP>), approximately solar metallicity star [log N(Fe)
  =-4.37 ± 0.06 dex or [Fe/H] = 0.05 ± 0.20 dex]. We measure a
  non-local thermodynamic equilibrium lithium abundance of log N(Li)
  = 3.1 ± 0.1 dex, which from depletion models gives rise to an age
  of 7? Myr for the system. Our measured chromospheric activity (? of
  -4.12) returns an age of 26 ± 2 Myr, as does fitting pre-main-sequence
  evolutionary tracks (τ<SUB>evol</SUB>= 22 ± 3 Myr), both of these
  are in disagreement with the lithium age. We speculate on reasons
  for this difference and introduce new models for lithium depletion
  that incorporate both rotation and magnetic field effects. We also
  synthesize solar, metal-poor and metal-rich substellar evolutionary
  models to better determine the bulk properties of PZ Tel B, showing
  that PZ Tel B is probably more massive than previous estimates, meaning
  the companion is not a giant exoplanet, even though a planetary-like
  formation origin can go some way to describing the distribution of
  benchmark binaries currently known. We show how PZ Tel B compares
  to other currently known age and metallicity benchmark systems and
  try to empirically test the effects of dust opacity as a function of
  metallicity on the near-infrared colours of brown dwarfs. Current models
  suggest that in the near-infrared observations are more sensitive to
  low-mass companions orbiting more metal rich stars. We also look for
  trends between infrared photometry and metallicity amongst a growing
  population of substellar benchmark objects, and identify the need for
  more data in mass-age-metallicity parameter space.

---------------------------------------------------------
Title: High-Resolution Spectroscopy of the Cool R CrB Star Candidates
    V1983 Cyg and V2074 Cyg
Authors: Smirnova, O.; Začs, L.; Pavlenko, Y. V.
2011ASPC..445..177S    Altcode:
  Preliminary results of high-resolution optical spectral analysis
  of two carbon-rich long-term variables, V1983 Cyg and V2047 Cyg,
  are presented. The stars were suspected to be cool R CrB variables
  according to their photometric light curves, although our spectroscopic
  study suggests that both stars are more similar to ordinary N-type
  carbon stars. For V1983 Cyg, possible absorption in the Balmer lines
  is detected.

---------------------------------------------------------
Title: Theory of azimuthal surface waves propagating in non-uniform
    waveguides
Authors: Girka, V. O.; Girka, I. O.; Girka, A. V.; Pavlenko, I. V.
2011JPlPh..77..493G    Altcode:
  This paper is devoted to the theory of surface waves propagating
  across axis of symmetry in non-uniform cylindrical metal waveguides
  with plasma filling. The presented results are devoted to: first,
  studying an influence of plasma density non-uniformity on the features
  of these waves; second, studying an influence of an external magnetic
  fields' non-uniformity on their dispersion properties; third, studying
  possibility to sustain gas discharge by propagation of these waves
  under different operating regimes. The problems have been solved both
  analytically and numerically. Plasma particles are described in the
  framework of hydrodynamics; fields of the studied waves are determined
  by a set of Maxwell equations. Analytical research of the obtained
  equations is carried out by the method of successive approximation;
  adequacy of such approach is proved here as well. Numerical evaluations
  of the possibilities to observe experimentally the phenomena, which
  accompany propagation of these waves, are carried out.

---------------------------------------------------------
Title: Spectroscopic Analysis of Cool Galactic R CrB Star Candidates
Authors: Smirnova, O.; Zavcs, L.; Pavlenko, Y. V.; Kaminsky, B.
2011IAUS..280P.340S    Altcode:
  The results of optical spectra analysis of two carbon-rich long-period
  variables V1983 Cyg and V2047 Cyg are presented. The stars were
  suspected to be cool R CrB variables candidates according to the
  photometric light curves. We compared the spectroscopic properties
  of the selected stars with those of DY Per and ordinary carbon
  stars to check their possible connection to cool RCBs. Also the
  spectral synthesis technique was used for analysis of the obtained
  high-resolution spectra, dominated by strong absorption features
  of carbon-bearing molecules. Our spectroscopic study suggests that
  both stars are more similar to ordinary N-type carbon stars than to
  DY Per star. For V1983 Cyg star possible absorption in Balmer lines
  is detected.

---------------------------------------------------------
Title: Infrared Mn I laboratory oscillator strengths for the study
    of late type stars and ultracool dwarfs
Authors: Blackwell-Whitehead, R.; Pavlenko, Y. V.; Nave, G.; Pickering,
   J. C.; Jones, H. R. A.; Lyubchik, Y.; Nilsson, H.
2011A&A...525A..44B    Altcode:
  <BR /> Aims: The aim of our new laboratory measurements is to measure
  accurate absolute oscillator strengths for neutral manganese transitions
  in the infrared needed for the study of late-type stars and ultracool
  dwarfs. <BR /> Methods: Branching fractions have been measured by high
  resolution Fourier transform spectroscopy and combined with radiative
  level lifetimes in the literature to yield oscillator strengths. <BR
  /> Results: We present experimental oscillator strengths for 20 Mn
  I transitions in the wavelength range 3216 to 13 997 Å, 15 of which
  are in the infrared. The transitions at 12 899 Å and 12 975 Å are
  observed as strong features in the spectra of late-type stars and
  ultracool dwarfs. We have fitted our calculated spectra to the observed
  Mn I lines in spectra of late-type stars. Using the new experimentally
  measured Mn I log(gf) values together with existing data for Mn I
  hyperfine structure splitting factors we determined the manganese
  abundance to be log N(Mn) = -6.65 ± 0.05 in the atmosphere of the Sun,
  log N(Mn) = 6.95 ± 0.20 in the atmosphere of Arcturus, and log N(Mn)
  = -6.70 ± 0.20 in the atmosphere of M 9.5 dwarf 2MASSW 0140026+270150.

---------------------------------------------------------
Title: Spectral Investigations of CM Dra
Authors: Kuznetsov, M. K.; Pavlenko, Y. V.; Pinfield, D.; Jones, H.
2010OAP....23...74K    Altcode:
  We present an analysis of a high resolution (R=47000) echelle spectra
  of the low-mass eclipsing binary CM Draconis, which were obtained on
  the 4.2-m William Herschel Telescope. Spectra were obtained for various
  phases of the orbit. There are some difficulties in echelle spectra
  processing of cool stars, since it is hard to get energy distribution
  in a large scale in such spectra. We proposed an efficient method
  for making the continuum of spectrum of cool stars. We refined the
  parameters (effective temperature, rotational velocity and metallicity)
  of the components of the system CM Dra using the method of stellar
  atmospheres. The data that we obtained are in good agreement with the
  results obtained by other authors. It is indicate on efficiency of our
  technique. The errors of temperature and metallicity determinations
  is about 100 K and 0.3 dex respectively.

---------------------------------------------------------
Title: Line Identification And Equivalent Width Measurements Of
    Atomic Lines In Spectra Of 40 Late M Dwarfs
Authors: Deshpande, Rohit; Martin, E. L.; Montgomery, M. M.; Lyubchik,
   Y.; Zapatero Osorio, M. R.; Rodler, F.; del Burgo, C.; Pavlenko, Y.
2010AAS...21560604D    Altcode: 2010BAAS...36R1130D
  We present preliminary results of line identification and equivalent
  width measurements in spectra of late M Dwarfs. We obtained 3.5
  nights on Keck NASA time to collect high resolution (R 20,000)
  near-infrared (J-band) spectra using the NIRSPEC instrument on the
  Keck II telescope. Our sample consists of 40 nearby (distance &lt;
  20 pc) late M dwarfs (spectral type M5 - M9.5). Using VALD database
  we identified new atomic lines and verified them by comparing our
  results to those obtained through models of synthetic spectra. We
  obtained equivalent width of new and previously observed atomic
  lines. Our results of existing atomic lines compare well with those
  from Cushing et al. 2005. We observe a linearly increasing trend in
  equivalent widths of strong lines such as K I l while a decreasing
  trend is found in weakening lines like Na I.

---------------------------------------------------------
Title: Rotational Velocities for M Dwarfs
Authors: Jenkins, J. S.; Ramsey, L. W.; Jones, H. R. A.; Pavlenko,
   Y.; Gallardo, J.; Barnes, J. R.; Pinfield, D. J.
2009ApJ...704..975J    Altcode: 2009arXiv0908.4092J
  We present spectroscopic rotation velocities (v sin i) for 56 M dwarf
  stars using high-resolution Hobby-Eberly Telescope High Resolution
  Spectrograph red spectroscopy. In addition, we have also determined
  photometric effective temperatures, masses, and metallicities ([Fe/H])
  for some stars observed here and in the literature where we could
  acquire accurate parallax measurements and relevant photometry. We
  have increased the number of known v sin i values for mid M stars
  by around 80% and can confirm a weakly increasing rotation velocity
  with decreasing effective temperature. Our sample of v sin is peak
  at low velocities (~3 km s<SUP>-1</SUP>). We find a change in the
  rotational velocity distribution between early M and late M stars,
  which is likely due to the changing field topology between partially
  and fully convective stars. There is also a possible further change
  in the rotational distribution toward the late M dwarfs where dust
  begins to play a role in the stellar atmospheres. We also link v
  sin i to age and show how it can be used to provide mid-M star age
  limits. When all literature velocities for M dwarfs are added to our
  sample, there are 198 with v sin i &lt;= 10 km s<SUP>-1</SUP> and 124
  in the mid-to-late M star regime (M3.0-M9.5) where measuring precision
  optical radial velocities is difficult. In addition, we also search
  the spectra for any significant Hα emission or absorption. Forty three
  percent were found to exhibit such emission and could represent young,
  active objects with high levels of radial-velocity noise. We acquired
  two epochs of spectra for the star GJ1253 spread by almost one month
  and the Hα profile changed from showing no clear signs of emission,
  to exhibiting a clear emission peak. Four stars in our sample appear
  to be low-mass binaries (GJ1080, GJ3129, Gl802, and LHS3080), with
  both GJ3129 and Gl802 exhibiting double Hα emission features. The
  tables presented here will aid any future M star planet search target
  selection to extract stars with low v sin i. <P />Based on observations
  obtained with the Hobby-Eberly Telescope, which is a joint project of
  the University of Texas at Austin, the Pennsylvania State University,
  Stanford University, Ludwig-Maximilians-Universität München, and
  Georg-August-Universität Göttingen.

---------------------------------------------------------
Title: Model Atmospheres and Spectra of Peculiar Stars
Authors: Pavlenko, Y. V.; Evans, A.; Duerbeck, H. W.; Geballe, T.;
   Yakovina, L.; Kaminsky, B.; Kerr, T.
2008ASPC..401..124P    Altcode: 2009ASPC..401..124P
  The method and results of the computation of the model atmospheres
  and spectral energy distributions of chemically peculiar stars
  are discussed. The models and spectra are computed with special
  consideration of the particular problems encountered for peculiar
  and hydrogen deficient stars in the later stages of evolution. We
  present some computed model atmospheres and fits to observed spectra
  of Sakurai's object, V838 Mon, and RS Oph.

---------------------------------------------------------
Title: Fifteen new T dwarfs discovered in the UKIDSS Large Area Survey
Authors: Pinfield, D. J.; Burningham, B.; Tamura, M.; Leggett, S. K.;
   Lodieu, N.; Lucas, P. W.; Mortlock, D. J.; Warren, S. J.; Homeier,
   D.; Ishii, M.; Deacon, N. R.; McMahon, R. G.; Hewett, P. C.; Osori,
   M. R. Zapatero; Martin, E. L.; Jones, H. R. A.; Venemans, B. P.;
   Day-Jones, A. C.; Dobbie, P. D.; Folkes, S. L.; Dye, S.; Allard, F.;
   Baraffe, I.; Barrado Y Navascués, D.; Casewell, S. L.; Chiu, K.;
   Chabrier, G.; Clarke, F.; Hodgkin, S. T.; Magazzù, A.; McCaughrean,
   M. J.; Nakajima, T.; Pavlenko, Y.; Tinney, C. G.
2008MNRAS.390..304P    Altcode: 2008arXiv0806.0294P
  We present the discovery of 15 new T2.5-T7.5 dwarfs (with estimated
  distances ~24-93pc), identified in the first three main data releases
  of the United Kingdom Infrared Telescope (UKIRT) Infrared Deep Sky
  Survey. This brings the total number of T dwarfs discovered in the
  Large Area Survey (LAS) (to date) to 28. These discoveries are confirmed
  by near-infrared spectroscopy, from which we derive spectral types on
  the unified scheme of Burgasser et al. Seven of the new T dwarfs have
  spectral types of T2.5-T4.5, five have spectral types of T5-T5.5, one is
  a T6.5p and two are T7-7.5. We assess spectral morphology and colours
  to identify T dwarfs in our sample that may have non-typical physical
  properties (by comparison to solar neighbourhood populations), and find
  that three of these new T dwarfs may have unusual metallicity, two may
  have low surface gravity, and one may have high surface gravity. The
  colours of the full sample of LAS T dwarfs show a possible trend to
  bluer Y - J with decreasing effective temperature, and some interesting
  colour changes in J - H and z - J (deserving further investigation)
  beyond T8. The LAS T dwarf sample from the first and second main data
  releases show good evidence for a good level of completion to J =
  19. By accounting for the main sources of incompleteness (selection,
  follow-up and spatial) as well as the effects of unresolved binarity,
  Malmquist and Eddington bias, we estimate that there are 17 +/- 4 &gt;=
  T 4 dwarfs in the J &lt;= 19 volume of the LAS second data release. This
  value is most consistent with theoretical predictions if the substellar
  mass function exponent α (dN/dm ~ m<SUP>-α</SUP>) lies between -1.0
  and 0. This is consistent with the latest 2-Micron All Sky Survey
  (2MASS)/Sloan Digital Sky Survey (SDSS) constraint (which is based
  on lower number statistics) and is significantly lower than the α ~
  1.0 suggested by L dwarf field populations, which is possibly a result
  of the lower mass range probed by the T dwarf class.

---------------------------------------------------------
Title: Model Atmospheres and Spectra for Cool Hydrogen-Deficient
    Stars and Peculiar Giants
Authors: Pavlenko, Y. V.
2008ASPC..391...65P    Altcode:
  New model atmospheres, spectra and spectral energy distributions
  of hydrogen-deficient chemically peculiar stars are presented. The
  methods used in the computation of these models are discussed, with
  special consideration given to the treatment of opacity. Some of the
  model atmospheres have been computed for R CrB stars with different
  H/He ratios and carbon abundances. In order to test these models the
  observed spectra of Sakurai's object and some carbon-rich giants are
  fit with the newly computed spectral energy distributions.

---------------------------------------------------------
Title: Metallicities and activities of southern stars
Authors: Jenkins, J. S.; Jones, H. R. A.; Pavlenko, Y.; Pinfield,
   D. J.; Barnes, J. R.; Lyubchik, Y.
2008A&A...485..571J    Altcode: 2008arXiv0804.1128J
  Aims: We present the results from high-resolution spectroscopic
  measurements to determine metallicities and activities of bright
  stars in the southern hemisphere. <BR />Methods: We measured the
  iron abundances ([Fe/H]'s) and chromospheric emission indices (log
  h{R}'<SUB>{HK</SUB>}) of 353 solar-type stars with V = 7.5-9.5. [Fe/H]
  abundances are determined using a custom χ<SUP>2</SUP> fitting
  procedure within a large grid of Kurucz model atmospheres. The
  chromospheric activities were determined by measuring the amount of
  emission in the cores of the strong Caii HK lines. <BR />Results: Our
  comparison of the metallicity sample to other [Fe/H] determinations
  was found to agree at the ±0.05 dex level for spectroscopic values
  and at the ±0.1 dex level for photometric values. The distribution
  of chromospheric activities is described by a bimodal distribution,
  agreeing with the conclusions from other works. Also an analysis of
  Maunder minimum status was attempted, and it was found that 6 ± 4 stars
  in the sample could be in a Maunder minimum phase of their evolution
  and hence the Sun should only spend a few per cent of its main sequence
  lifetime in Maunder minimum. <P />Based on observations made with the
  ESO telescopes at the La Silla Paranal observatory under programme ID's
  076.C-0578(B) and 077.C-0192(A). Table 4 is only available in electronic
  form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
  or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/485/571

---------------------------------------------------------
Title: VizieR Online Data Catalog: Metallicities &amp; activities
    of southern stars (Jenkins+, 2008)
Authors: Jenkins, J. S.; Jones, H. R. A.; Pavlenko, Y.; Pinfield,
   D. J.; Barnes, J. R.; Lyubchik, Y.
2008yCat..34850571J    Altcode:
  This table comprises a list of stellar metallicities and activities
  for a number of solar-type stars in the southern hemisphere using
  high-resolution (R~46000) spectra acquired at the ESO-MPI 2.2m telescope
  and the instrument FEROS. The stars all have B-V colours in the range
  0.5-0.9, V magnitudes between 7.5-9.5 and were selected from the
  Hipparcos catalogue (Perryman et al., 1997, Cat. ). The chromospheric
  activities along with their photon counting errors are shown, and were
  extracted by comparing the flux in triangular bandpasses centred in the
  cores of the Calcium II H and K lines (wavelengths of 3933.664{AA} and
  3968.470{AA}) against the flux in two square bandpass regions centred
  on the continuum at either side of these lines (wavelengths of 3891{AA}
  and 4001{AA}). These values have been calibrated onto the Mt. Wilson
  system of measurements (Duncan et al., 1991, Cat. ) and then converted
  to the commonly used logRhk system (Noyes et al. 1984ApJ...287..769N)
  to remove the photospheric component of the flux. The metallicities
  shown in column 6, were measured by comparing a grid of synthetic
  spectra (WITA6; Pavlenko et al., 1995A&amp;A...303..807P) to a number
  of mostly weak and unblended FeI lines at this spectral resolution. The
  internal errors were determined by fitting the Chi-squared parabola and
  after comparison with other works these values were found to agree to
  &lt;0.1dex or 0.05dex with other high-resolution spectral abundances
  (e.g. Valenti &amp; Fischer, 2005, Cat. ). The tail of objects with
  really high errors were mainly lower S/N spectra due to changing
  weather patterns. <P />(1 data file).

---------------------------------------------------------
Title: Spectral analysis of high resolution near-infrared spectra
    of ultra cool dwarfs
Authors: Lyubchik, Y.; Jones, H. R. A.; Pavlenko, Y. V.; Martin, E.;
   McLean, I. S.; Prato, L.; Barber, R. J.; Tennyson, J.
2007A&A...473..257L    Altcode: 2007arXiv0708.2676L
  Aims:We present an analysis of high resolution spectra in the J band
  of five ultra cool dwarfs from M6 to L0. <BR />Methods: We make use
  of a new ab initio water vapour line list and existing line lists of
  FeH and CrH for modelling the observations. <BR />Results: We find a
  good fit for the Mn I 12 899.76 Å line. This feature is one of the
  few for which we have a reliable oscillator strength. Other atomic
  features are present but most of the observed features are FeH and
  H2O lines. While we are uncertain about the quality of many of the
  atomic line parameters, the FeH and CrH line lists predict a number
  of features which are not apparent in our observed spectra. We infer
  that the main limiting factor in our spectral analysis is the FeH and
  CrH molecular spectra.

---------------------------------------------------------
Title: Eight new T4.5-T7.5 dwarfs discovered in the UKIDSS Large
    Area Survey Data Release 1
Authors: Lodieu, N.; Pinfield, D. J.; Leggett, S. K.; Jameson, R. F.;
   Mortlock, D. J.; Warren, S. J.; Burningham, B.; Lucas, P. W.; Chiu,
   K.; Liu, M. C.; Venemans, B. P.; McMahon, R. G.; Allard, F.; Baraffe,
   I.; Barrado y Navascués, D.; Carraro, G.; Casewell, S. L.; Chabrier,
   G.; Chappelle, R. J.; Clarke, F.; Day-Jones, A. C.; Deacon, N. R.;
   Dobbie, P. D.; Folkes, S. L.; Hambly, N. C.; Hewett, P. C.; Hodgkin,
   S. T.; Jones, H. R. A.; Kendall, T. R.; Magazzù, A.; Martín, E. L.;
   McCaughrean, M. J.; Nakajima, T.; Pavlenko, Y.; Tamura, M.; Tinney,
   C. G.; Zapatero Osorio, M. R.
2007MNRAS.379.1423L    Altcode: 2007MNRAS.tmp..609L; 2007arXiv0705.3727L
  We present eight new T4.5-T7.5 dwarfs identified in the UKIRT
  (United Kingdom Infrared Telescope) Infrared Deep Sky Survey (UKIDSS)
  Large Area Survey (LAS) Data Release 1 (DR1). In addition we have
  recovered the T4.5 dwarf SDSSJ020742.91+000056.2 and the T8.5 dwarf
  ULASJ003402.77-005206.7. Photometric candidates were picked up in
  two-colour diagrams over 190deg<SUP>2</SUP> (DR1) and selected in at
  least two filters. All candidates exhibit near-infrared spectra with
  strong methane and water absorption bands characteristic of T dwarfs
  and the derived spectral types follow the unified scheme of Burgasser
  et al.. We have found six new T4.5-T5.5 dwarfs, one T7 dwarf, one T7.5
  dwarf and recovered a T4.5 dwarf and a T8.5 dwarf. We provide distance
  estimates which lie in the 15-85pc range; the T7.5 and T8.5 dwarfs are
  probably within 25pc of the Sun. We conclude with a discussion of the
  number of T dwarfs expected after completion of the LAS, comparing these
  initial results to theoretical simulations. <P />Based on observations
  made with the United Kingdom Infrared Telescope, operated by the Joint
  Astronomy Centre on behalf of the UK Particle Physics and Astronomy
  Research Council. <P />E-mail: nlodieu@iac.es ‡ <P />Alfred P. Sloan
  Research Fellow.

---------------------------------------------------------
Title: Two T dwarfs from the UKIDSS early data release
Authors: Kendall, T. R.; Tamura, M.; Tinney, C. G.; Martín, E. L.;
   Ishii, M.; Pinfield, D. J.; Lucas, P. W.; Jones, H. R. A.; Leggett,
   S. K.; Dye, S.; Hewett, P. C.; Allard, F.; Baraffe, I.; Barrado Y
   Navascués, D.; Carraro, G.; Casewell, S. L.; Chabrier, G.; Chappelle,
   R. J.; Clarke, F.; Day-Jones, A.; Deacon, N.; Dobbie, P. D.; Folkes,
   S.; Hambly, N. C.; Hodgkin, S. T.; Nakajima, T.; Jameson, R. F.;
   Lodieu, N.; Magazzù, A.; McCaughrean, M. J.; Pavlenko, Y. V.; Tadashi,
   N.; Zapatero Osorio, M. R.
2007A&A...466.1059K    Altcode: 2007astro.ph..2534K
  Context: We report on the first ultracool dwarf discoveries from the
  UKIRT Infrared Deep Sky Survey (UKIDSS) Large Area Survey Early Data
  Release (LAS EDR), in particular the discovery of T dwarfs which
  are fainter and more distant than those found using the 2MASS and
  SDSS surveys. <BR />Aims: We aim to show that our methodologies for
  searching the ~27 deg<SUP>2</SUP> of the LAS EDR are successful for
  finding both L and T dwarfs via cross-correlation with the Sloan
  Digital Sky Survey (SDSS) DR4 release. While the area searched so
  far is small, the numbers of objects found shows great promise for
  near-future releases of the LAS and great potential for finding large
  numbers of such dwarfs. <BR />Methods: Ultracool dwarfs are selected
  by combinations of their YJH(K) UKIDSS colours and SDSS DR4 z-J and
  i-z colours, or, lower limits on these red optical/infrared colours
  in the case of DR4 dropouts. After passing visual inspection tests,
  candidates have been followed up by methane imaging and spectroscopy
  at 4 m and 8 m-class facilities. <BR />Results: Our main result is the
  discovery following CH4 imaging and spectroscopy of a T4.5 dwarf, ULAS
  J 1452+0655, lying ~80 pc distant. A further T dwarf candidate, ULAS J
  1301+0023, has very similar CH4 colours but has not yet been confirmed
  spectroscopically. We also report on the identification of a brighter
  L0 dwarf, and on the selection of a list of LAS objects designed to
  probe for T-like dwarfs to the survey J-band limit. <BR />Conclusions:
  Our findings indicate that the combination of the UKIDSS LAS and SDSS
  surveys provide an excellent tool for identifying L and T dwarfs down
  to much fainter limits than previously possible. Our discovery of
  one confirmed and one probable T dwarf in the EDR is consistent with
  expectations from the previously measured T dwarf density on the sky.

---------------------------------------------------------
Title: Modelling the Spectrum and SED of V838 Mon
Authors: Pavlenko, Y.; Kaminsky, B.; Lyubchik, Y.; Yakovina, L.
2007ASPC..363..225P    Altcode: 2006astro.ph..9604P
  We model the spectra and spectral energy distribution of V838 Mon which
  were observed in February, March, and November, 2002. Theoretical
  spectra are calculated using the classical model atmospheres taking
  into account absorption of atomic and molecular lines. By fitting the
  observed spectra we determine the physical parameters of the atmosphere
  of V838 Mon. These parameters are determined to be {T<SUB>eff</SUB> }
  = 5330 ± 300 K, 5540 ± 270 K, 4960 ± 190 K, and 2000 ± 200 K for
  February 25, March 2, March 26, and November 6, respectively.

---------------------------------------------------------
Title: Experimental TiI oscillator strengths and their application
    to cool star analysis
Authors: Blackwell-Whitehead, R. J.; Lundberg, H.; Nave, G.; Pickering,
   J. C.; Jones, H. R. A.; Lyubchik, Y.; Pavlenko, Y. V.; Viti, S.
2006MNRAS.373.1603B    Altcode: 2006astro.ph.12656B; 2006MNRAS.tmp.1308B
  We report experimental oscillator strengths for 88 TiI transitions
  covering the wavelength range 465-3892 nm, 67 of which had no previous
  experimental values. Radiative lifetimes for 13 energy levels, including
  the low energy levels 3d<SUP>2</SUP>(<SUP>3</SUP>F) 4s4p (<SUP>3</SUP>P)
  z <SUP>5</SUP>D°<SUB>j</SUB>, have been measured using time-resolved
  laser-induced fluorescence. Intensity-calibrated TiI spectra have been
  measured using Fourier transform spectroscopy to determine branching
  fractions for the decay channels of these levels. The branching
  fractions are combined with the radiative lifetimes to yield absolute
  transition probabilities and oscillator strengths. Our measurements
  include 50 transitions in the previously unobserved infrared region
  λ &gt; 1.0μm, a region of particular interest to the analysis of
  cool stars and brown dwarfs.

---------------------------------------------------------
Title: Theoretical modelling of optical and IR spectra of brown
    dwarfs and ultracool dwarfs
Authors: Pavlenko, Y. V.
2005AN....326..934P    Altcode:
  The current state of theoretical modelling of the spectra of cool
  dwarfs and ultracool objects are discussed. Fits of synthetical spectral
  energy distributions (SEDs) in the optical and IR spectral regions to
  observed spectra show problems of theoretical modelling. Problems of
  interpretation of observed spectra are more obvious for the case of L
  and T dwarfs. Still even for late-M dwarfs the situation is far from
  being perfect. Some examples of the fine analysis of the spectra of
  ultracool dwarfs are presented.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Linelist of HCN and HNC (Harris+,
    2006)
Authors: Harris, G. J.; Tennyson, J.; Kaminskiy, B.; Pavlenko, Y. V.;
   Jones, H. R. A.
2005yCat.6121....0H    Altcode:
  We present an energy level list which contains the ab initio energies
  and exact quantum numbers from HPT, together with lab determined
  energies and assigned approximate quantum numbers where available. A
  new HCN/HNC linelist is presented. Lab determined energy levels were
  used to compute accurate line frequencies, where available. Where
  lab data is not available frequencies are computed from ab initio
  energy levels. The linelist is truncated at a minimum frequency of
  3*10-28^cm/mol at T=3000K. Resulting in a linelist of 38 million
  lines, which accounts for 99.99% of the opacity of the full linelist
  at 3000K. The file has been compressed using bzip2. The data is sorted
  into increasing frequency order. A FORTRAN code is supplied to convert
  the Einstein A coefficients of HPT and the new energy level list into
  a usable linelist. <P />(3 data files).

---------------------------------------------------------
Title: Temperatures in the atmopshere of the cool component of
    CH Cygni
Authors: Jurdana-Sepic, R.; Kotnik-Karuza, D.; Majlinger, Z.; Pavlenko,
   Y. V.
2004ASPC..318..371J    Altcode: 2004ssrc.conf..371J
  We have investigated the temperatures in the atmosphere of the cool
  component of CH Cygni by use of highly resolved optical and near
  infrared spectra taken in a short epoch of the 1998-2000 active
  phase. TiO absorption bands belonging to α, γ, γ', β, δ, φ and
  ɛ band systems with partly resolved rotational structure have been
  studied and vibrational temperatures belonging to γ' and φ system
  were obtained from the relative intensities of vibrational band
  heads. In order to determine the effective temperature we used model
  atmospheres appropriate for M giants and computed synthetic spectra
  by the line-to-line approach. Results are discussed in view of the
  previously determined rotational temperature.

---------------------------------------------------------
Title: Atomic lines in infrared spectra for ultracool dwarfs
Authors: Lyubchik, Y.; Jones, H. R. A.; Pavlenko, Y. V.; Viti, S.;
   Pickering, J. C.; Blackwell-Whitehead, R.
2004A&A...416..655L    Altcode: 2003astro.ph.12578L
  We provide a set of atomic lines which are suitable for the description
  of ultracool dwarf spectra from 10 000 to 25 000 Å. This atomic
  linelist was made using both synthetic spectra calculations and existing
  atlases of infrared spectra of Arcturus and Sunspot umbra. We present
  plots which show the comparison of synthetic spectra and observed
  Arcturus and Sunspot umbral spectra for all atomic lines likely to
  be observable in high resolution infrared spectra. <P />Figure 1
  is only available in electronic form at http://www.edpsciences.org
  <P />Tables 1 and 2 are only available in electronic form at the
  CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via
  http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/416/655

---------------------------------------------------------
Title: Draco 461, an intrinsic carbon star in a metal poor stellar
population: 3<SUP>rd</SUP> dredge up and mixing
Authors: Domínguez, I.; Abia, C.; Straniero, O. Cristallo, S.;
   Pavlenko, Y. V.
2004MmSAI..75..601D    Altcode:
  In July 2003 we observed the first Li-rich carbon star in a dwarf
  spheroidal galaxy. We compute stellar models for AGB stars and, by
  comparing them to the available photometric and spectroscopic data,
  conclude that D461 is an intrinsic carbon star, more massive and
  younger than the dominant stellar population of Draco.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Atomic lines in IR spectra for
    ultracool dwarfs (Lyubchik+, 2004)
Authors: Lyubchik, Y.; Jones, H. R. A.; Pavlenko, Y. V.; Viti, S.;
   Pickering, J. C.; Blackwell-Whitehead, R.
2004yCat..34160655L    Altcode:
  Table 1 contains all identified lines with central intensities
  deeper than 0.8 of residual flux using "ultracool dwarf model"
  identifications. <P />Table 2 investigates the sensitivity of priority 1
  lines identified in Table 1 to temperature, gravity and metallicity. <P
  />We compute some synthetic spectra for ultracool objects varying
  parameters of Teff, log g and metallicity to show the sensitivity of
  the central intensities of identified lines to these parameters. For
  our computations we chose the minimal step in model atmospheres grid:
  {Delta}Teff=100K, {Delta}logg=0.5, {Delta}[M/H]=-0.5. STeff shows the
  dependence of residual fluxes on effective temperature. For comparison a
  2100/5.0/0.0 synthetic spectrum was used. One can see that only a few
  lines show strong temperature dependence for {Delta}=100K. <P />The
  NextGen 2000/4.5/0.0 model was used with 2000/5.0/0.0 to test gravity
  sensitivity. The dependence for {Delta}(log g)=0.5 is also relatively
  weak for most lines. <P />The NextGen model atmospheres 2000/5.0/-0.5
  and 2000/5.0/0.0 to test metallicity sensitivity. The metallicity
  dependence is relatively high for all lines. <P />(2 data files).

---------------------------------------------------------
Title: A Comparison of Water Vapour Line Lists
Authors: Jones, H. R. A.; Pavlenko, Y.; Viti, S.; Tennyson, J.
2003csss...12..899J    Altcode:
  M dwarf spectra, at wavelengths beyond 1.35 μm, are dominated by water
  vapour yet terrestrial water vapour makes it notoriously difficult to
  make accurate measurement from ground-based observations. We have used
  the short wavelength spectrometer on the Infrared Space Observatory
  to obtain the 2.5--3.0 μm region. The observations show a good
  match with synthetic spectra based on the Partridge &amp; Schwenke
  (1997) line list though not with the SCAN (Jorgensen et al. 2001)
  line list. Nonetheless, the Partridge &amp; Schwenke calculations for
  water vapour lines still need to be extended to higher energy levels
  with good convergence for reliable modelling of hot water vapour. Then
  water bands can assume their natural role as the primary tool for the
  spectroscopic analysis of M stars.

---------------------------------------------------------
Title: Model Atmospheres and SEDs of Chemically Peculiar Stars
Authors: Pavlenko, Y. V.
2003IAUS..210P.A16P    Altcode: 2002astro.ph..9022P
  Procedure and results of computations of stellar model atmospheres and
  spectral energy distributions are discussed. Model atmospheres of some
  chemically peculiar stars are computed taking into account detailed
  information about their abundances: -- R CrB-like stars of Teff $\sim$
  7000 K, -- Sakurai's object (V4334 Sgr) of 4000 $&lt;$ \Tef $&lt;$
  7000 K -- Przybylski's star of Teff $\sim$ 6500 K. We show that our
  self-consistent approach provides a unique possibility to investigate
  the temporal changes of physical parameters of chemically peculiar
  stars. Some problems of computation of model atmospheres of M and
  C-giants are also considered.

---------------------------------------------------------
Title: Stellar Abundance Patterns. What is the Possible Level of
    Completeness Today?
Authors: Gopka, V.; Yushchenko, A.; Musaev, F.; Galazutdinov, G.;
   Kim, C.; Shavrina, A.; Pavlenko, Y.; Polosukhina, N.; North, P.
2003IAUS..210P..E5G    Altcode: 2003astro.ph..8339G
  We discuss the way of increasing of the number of chemical elements,
  investigated in stellar spectra. We can reach it by using spectrum
  synthesis method, new atomic data and observation of stellar spectra
  with resolution comparable to solar spectral atlases. We show two
  examples of this kind researches. The first is the implementation
  of new atomic data to well known Przybylski's star. We show that the
  number of spectral lines, which can be identificated in the spectrum
  of this star can be significantly higher. The second example is the
  investigation of zeta Cyg. We found the abundances of 51 elements in
  the atmosphere of this mild barium star.

---------------------------------------------------------
Title: Carbon monoxide bands in M dwarfs
Authors: Pavlenko, Y. V.; Jones, H. R. A.
2002A&A...396..967P    Altcode: 2002astro.ph.10017P
  We compare the observational and theoretical spectra of the Delta v
  = 2 CO bands in a range of M dwarfs. We investigate the dependence
  of theoretical spectra on effective temperatures as well as carbon
  abundance. In general we find that the synthetic CO bands fit the
  observed data extremely well and are excellent diagnostics. In
  particular the synthetic spectra reasonably match observations and
  the best fit temperatures are similar to those found by empirical
  methods. We also examine the <SUP>12</SUP>C/<SUP>13</SUP>C isotopic
  ratio. We find that fundamental <SUP>13</SUP>CO bands around 2.345 and
  2.375 mu m are good discriminators for the <SUP>12</SUP>C/<SUP>13</SUP>C
  ratio in M dwarfs. The 2.375 mu m band is more useful because it doesn't
  suffer such serious contamination by water vapour transitions. Our
  current dataset does not quite have the wavelength coverage to perform
  a reliable determination of the <SUP>12</SUP>C/<SUP>13</SUP>C ratio in
  M dwarfs. For this we recommend observing the region 2.31-2.40 mu m
  at a resolution of better than 1000. Alternatively the observational
  problems of contamination by water vapour at 2.345 mu m maybe solved
  by observing at resolutions of around 50 000. We also investigated the
  possibility of using the Delta v = 1 CO bands around 4.5 mu m. We find
  that the contamination due to water vapour is even more of a problem
  at these wavelengths.

---------------------------------------------------------
Title: Models of infrared spectra of Sakurai's Object (V4334 Sgr)
    in 1997
Authors: Pavlenko, Y. V.; Geballe, T. R.
2002A&A...390..621P    Altcode: 2002astro.ph..5528P
  Theoretical spectral energy distributions computed for a grid
  of hydrogen-deficient and carbon-rich model atmospheres have been
  compared with the observed infrared (1-2.5 mu m) spectra of V4334 Sgr
  (Sakurai's Object) on 1997 April 21 and July 13. The comparison yields
  an effective temperature of T<SUB>eff</SUB> = 5500 +/- 200 K for the
  April date and T<SUB>eff</SUB> = 5250 +/- 200 K for July. The observed
  spectra are well fitted by Asplund et al. (\cite{Asplund99}) abundances,
  except that the carbon abundance is higher by 0.3 dex. Hot dust produces
  significant excess continuum at the long wavelength ends of the 1997
  spectra. Based on observations obtained at the United Kingdom Infrared
  Telescope (UKIRT), which is operated by the Joint Astronomy Centre on
  behalf of the U. K. Particle Physics and Astronomy Research Council.

---------------------------------------------------------
Title: Formation of the Optical Spectra of L Dwarfs
Authors: Pavlenko, Y.
2001udns.conf...33P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: About Use of Quantum Effects and Fundamental Physical
    Constants for Elaboration of the Measurement Standards in the Field
    of Electronic Measurements
Authors: Niemeyer, J.; Pavlenko, Y.; Anikin, V.; Kolbasin, A.;
   Seredniy, V.
2001pems.conf..341N    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Formation of the Optical Spectra of the Coolest M- and L-dwarfs
    and Lithium Abundances in their Atmospheres
Authors: Pavlenko, Y. V.
2000IAUS..198..454P    Altcode: 2000astro.ph..2144P
  Theoretical aspects of modeling of spectra of late M- and L-dwarfs are
  discussed. We show, that the processes of formation of spectra of M-
  and L-dwarfs are basically different. Instead of the case of M-dwarfs,
  atoms of Ti and V should be depleted into grains in the atmospheres
  of L-dwarfs. Overall shape of the L-dwarf spectra is governed by
  the K I + Na I resonance line wings of the huge strength. To fit
  lithium lines observed in spectra of the coolest dwarfs we used
  two additional suggestions: a) there are some EXTRA depletions of
  molecular species absorbed in the optical spectra of L-dwarfs; b)
  there may be (a few?) additional (“dusty”?) opacity sources in their
  atmospheres. Problems of lithium line formation and the “natural”
  limitation of their use for the “lithium test” for the case of
  L-dwarfs are considered.

---------------------------------------------------------
Title: The formation of lithium lines in the atmospheres of super
    Li-rich AGB stars
Authors: Abia, C.; Pavlenko, Y.; de Laverny, P.
1999A&A...351..273A    Altcode: 1999astro.ph..4420A
  The formation of lithium lines in the atmosphere of C-rich giants is
  discussed. LTE and NLTE approximations are used to model lithium lines
  in the spectra of super Li-rich AGB stars. The system of equations
  of the statistical balance of neutral Li in plane-parallel model
  atmospheres is solved for a 20-level atom model. JOLA and line-by-line
  models of molecular absorption are used to compute synthetic spectra as
  well as the opacity in the frequencies of bound-bound and bound-free
  transitions of the lithium lines. Curves of growth and synthetic
  spectra are computed in LTE and NLTE for several model atmospheres
  of different {T_eff} and C/O ratios for four lithium absorptions,
  namely: the lambda 4603, lambda 6104, lambda 6708 and lambda 8126 Å
  Li I lines. The sensitivity of NLTE effects on {T_eff} and the C/O
  ratio is discussed. We found that NLTE mainly affects the resonance
  line doublet (lambda6708 ) while the impact of NLTE effects on the
  lithium subordinate lines, formed in the inner regions of C-rich
  giant atmospheres, is rather weak. Therefore the use of these lines is
  recommended for Li determination in AGB stars. However, in no case can
  we properly account for the formation of Li lines in AGB stars until
  sphericity, velocity stratifications, dust, chromospheres and other
  related phenomena, which are in fact present in AGB star atmospheres,
  are considered. Our results are used to derive Li abundances in three
  super-Li rich C-stars taking into account NLTE effects. Finally, the
  net Li yield from this class of stars into the interstellar medium
  is reconsidered.

---------------------------------------------------------
Title: The Lithium Lines Formation in Brown Dwarf Atmospheres:
    Molecules, Chromospheres, NLTE
Authors: Pavlenko, Y. V.
1998ASPC..134..416P    Altcode: 1998bdep.conf..416P
  No abstract at ADS

---------------------------------------------------------
Title: Ultraviolet NH bands as indicators of nitrogen abundance in
    the atmospheres of cool stars.
Authors: Yakovina, L. A.; Pavlenko, Y. V.
1998KPCB...14..195Y    Altcode:
  Nitrogen abundance indicators were selected for spectral resolutions
  of 0.0025 nm and 0.02 nm in the NH band region at λ336 nm. For this
  purpose a list of atomic lines from LOWLINES, DAT (CD-ROM No. 1 in
  Kurucz's 1993 database) and lists of molecular lines from CD-ROM
  No. 18 were tested and corrected using the spectrum of the Sun as
  a star. The effect of line list completeness on nitrogen abundance
  estimates is examined.

---------------------------------------------------------
Title: New and accurate Li abundance determinations in super Li-rich
    AGB stars
Authors: Abia, C.; de Laverny, P.; Pavlenko, Y.
1998IAUS..191P.101A    Altcode:
  Super lithium-rich AGB stars constitute the sole observational evidence
  of a stellar production of lithium. Abundance determinations report
  values as high as Li/H ~10^{-7} in their atmospheres (i.e. more
  than 10-100 times the cosmic abundance), therefore these stars might
  represent an important source of lithium in the galaxies. However most
  of these abundance analyses are based on the study of the resonance line
  of LiI 6708 Angstroms which usually is very strong or near saturation
  even in AGB stars with normal lithium abundances. Here we have used
  high-resolution and high signal-to-noise ratio spectra of three
  well known super Li-rich carbon stars (WZ Cas, WX Cyg and IY Hya)
  to derive LTE/N-LTE lithium abundances using two other accessible
  less-intense Li lines at 6103 and 8126 Angstroms for the first time
  in AGB stars. We show that N-LTE effects are very important for the
  resonance line. Furthermore, the core of the 6708 Angstroms line forms
  very high in the atmosphere of AGB stars where the structure of the
  atmosphere is almost unknown. That excludes the use of this line for
  realistic Li abundance determinations in AGB stars. On the contrary, we
  found that N-LTE effects are weak for the two other lines. Although it
  is saturated, the subordinate Li line at 8126 Angstroms is recommended
  to derive abundances in Li-rich AGB stars.

---------------------------------------------------------
Title: Common envelope evolution and Li in V471 Tauri.
Authors: Martin, E. L.; Pavlenko, Y.; Rebolo, R.
1997A&A...326..731M    Altcode:
  We have observed the spectral regions around the LiI resonance 670.8nm
  and subordinate 610.4nm lines of V471 Tau. This is an eclipsing post
  common-envelope (CE) binary system. A revision of several independent
  measurements of the parallax and proper motion of V471 Tau allow
  us to argue that this system is indeed a Hyades cluster member by
  examining and rejecting earlier, flawed results. Using spectral
  synthesis and taking into account NLTE effects, we have derived a
  photospheric Li abundance of log N(Li)=2.35+/-0.25 for the K dwarf,
  which is a factor &gt;100 higher than single Hyades members of the
  same mass. We argue that two mechanisms are responsible for this:
  a) Accretion of a substantial amount of Li-rich material onto the
  K dwarf during CE evolution inside the giant precursor of the white
  dwarf. Recently, a number of Li-rich giants have been observed and
  they appear to undergo large mass-loss. We speculate that CE evolution
  could actually explain the properties of these giants as well. b)
  Reduced Li depletion in the K dwarf due to sustained fast rotation
  in a short-period tidally-locked orbit. This process accounts for the
  preservation of Li after CE evolution has ceased.

---------------------------------------------------------
Title: Formation of lithium lines in very cool dwarfs.
Authors: Pavlenko, Y. V.; Rebolo, R.; Martin, E. L.; Garcia Lopez,
   R. J.
1995A&A...303..807P    Altcode:
  We present LTE and NLTE results on the formation of LiI lines (λ6103,
  λ6708, and λ8126) in the atmospheres of solar metallicity dwarfs with
  effective temperatures in the range 5500K to 2000K. NLTE effects are
  governed by overionization of Li and by the interlocking effects of
  energy levels. For stars with T_eff_&gt;=4000K, we confirm previous
  findings by Magazzu et al. (1992). NLTE corrections can lower the
  LTE Li abundances derived from strong LiIλ6708 lines by up to 0.5
  dex. Our computations using model atmospheres with T_eff_ between 3000K
  and 2000K show that prominent LiI lines are formed. We give a set of
  line profiles, which support the feasability of the Li test for brown
  dwarfs. The ionization-dissociation equilibrium for Li species was
  carefully considered. NLTE effects on the LiI lines of very cool dwarfs
  are found to be small, implying corrections to the LTE Li abundances
  lower than 0.1 dex. Several numerical tests have been carried out to
  estimate the effects of chromosphere-like structures on the formation
  of LiI lines. Our preliminary results suggest that in the presence of
  very strong chromospheres, the line strengths are reduced.

---------------------------------------------------------
Title: Li I Lines in POP II Dwarf Spectra: NLTE Effects
Authors: Pavlenko, Y. V.
1995lea..conf..324P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interpretations of stellar spectra: NLTE effects
Authors: Pavlenko, Y. V.
1995MmSAI..66..441P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interpretations of stellar spectra: NLTE effects
Authors: Pavlenko, Y. V.
1995HiA....10..453P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Behaviour of the Lithium Abundance Along the Pre-Main
    Sequence
Authors: Magazzú, A.; Martín, E. L.; Rebolo, R.; García Lopez,
   R. J.; Pavlenko, Y. V.
1995lea..conf..260M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Statistical Equilibrium of Lithium in the Atmospheres of
    Dwarfs with Various Metallicities
Authors: Pavlenko, Y. V.
1994AZh....71..600P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Beryllium abundances in unevolved metal deficient stars.
Authors: Rebolo, R.; Garcia Lopez, R. J.; Martin, E. L.; Beckman,
   J. E.; McKeith, C. D.; Webb, J. K.; Pavlenko, Y. V.
1993oee..conf..149R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Beryllium and Lithium abundances in stars with a range of
    metallicities
Authors: Garcia Lopez, R. J.; Martin, E. L.; Rebolo, R.; Beckman,
   J. E.; McKeith, C. D.; Webb, J. K.; Pavlenko, Y. V.
1993ASPC...40..180G    Altcode: 1993IAUCo.137..180G; 1993ist..proc..180G
  No abstract at ADS

---------------------------------------------------------
Title: Observational patterns of lithium depletion in pre-main
    sequence stars
Authors: Martín, E. L.; Rebolo, R.; Garcia Lopez, R. J.; Magazzu,
   A.; Pavlenko, Y. V.
1993ASPC...40..165M    Altcode: 1993ist..proc..165M; 1993IAUCo.137..165M
  No abstract at ADS

---------------------------------------------------------
Title: Nonlte Effects and Strong Lii Lines in the Spectra of the K
    Giants HD9746 and HD112127
Authors: Pavlenko, Y. V.
1992SvA....36..605P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Lithium Abundances in Classical and Weak T Tauri Stars
Authors: Magazzu, Antonio; Rebolo, Rafael; Pavlenko, Iakov V.
1992ApJ...392..159M    Altcode:
  A study on the lithium abundance in 36 T Tauri stars (mass range
  0.4-2.25 solar masses), partly based on high-dispersion spectra taken
  with the Isaac Newton Telescope, is presented. A study of non-LTE
  effects in the formation of the lithium double in T Tauri stars and
  derived corrections to the abundances in the LTE in the range 1.0-4.0
  log N(Li) is presented. Tor T(eff) of 400-4500 K, a significant upward
  correction to the LTE abundance (about 0.3-0.6 dex) is found. For
  T(eff) close to 500 K, smaller corrections (about 0.2 dex), and for
  log N(Li) greater than about 3, downward corrections (about 0.1 dex)
  are found. The initial value of the lithium abundance in T Tauri
  stars is estimated at 3.2 +/- 0.1, which is in close agreement with
  the accepted present cosmic abundance.

---------------------------------------------------------
Title: Statistical Equilibrium and the Lii 670.766-NM and 670.791-NM
    Absorption Lines in the Spectrum of Red Giants - Results
Authors: Pavlenko, Y. V.
1991SvA....35..623P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The statistical equilibrium and the 670.776- and 670.791-nm
    absorption lines of Li I in red-giant spectra - Methodology
Authors: Pavlenko, Y. V.
1991AZh....68..776P    Altcode:
  A method for calculating the statistical equilibrium for lithium in the
  atmospheres of red giants without LTE is analyzed. The cool-atmosphere
  opacity circulation method (absorption mean) is investigated. The
  analysis makes it possible to determine the role played by free-bound
  transitions from different levels in establishing the lithium ionization
  balance in the atmospheres of late stars.

---------------------------------------------------------
Title: Statistical Equilibrium and the 670.776-NM and 670.791-NM
    Lii Absorption Lines in the Spectrum of Red Giants - Procedure
Authors: Pavlenko, Y. V.
1991SvA....35..384P    Altcode:
  No abstract at ADS

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Title: Atmosphere of the K2III-STAR Alpha-Arietis
Authors: Berdyugina, S. V.; Boyarchuk, M. E.; Pavlenko, Y. V.; Savanov,
   I. S.; Shavrina, A. V.
1991SvA....35..387B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Determination of C N and O Abundances in the Atmospheres of
    Late Type Stars - Extreme Value Problem
Authors: Pavlenko, Y. V.
1991SvA....35..212P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The determination of C, N, and O abundances in late-type star
    atmospheres - Extremum problem
Authors: Pavlenko, Y. V.
1991AZh....68..431P    Altcode:
  The possibility of determining carbon, nitrogen, and oxygen abundances
  through the extremum problem treatment is discussed. The minimized
  functional consists of differences between observed and calculated
  parameters of atomic and molecular absorption lines or their blends. A
  brief description of the procedure and C, N, and O abundance data for
  the atmosphere of a K giant are presented.

---------------------------------------------------------
Title: Li C N and O Abundances and the 12/C/13/C Isotope Ratio in
    the Atmospheres of the K Giants 39-CYGNI and Alpha-Arietis
Authors: Boyarchuk, M. E.; Pavlenko, Y. V.; Shavrina, A. V.
1991SvA....35..143B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Spectral Features in the Circumstellar Envelope of the Close
    Binary System V367-CYGNI
Authors: Menchenkova, E. V.; Pavlenko, Y. V.
1990SvA....34..489M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The determination of physical parameters of the atmosphere
    of the primary star of the system V367 Cygni with the method of
    atmosphere models.
Authors: Menchenkova, E. V.; Pavlenko, Y. V.
1989AZh....66..194M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solution of the NLTE Problem for MGI in Atmosphere of M Giants
    with Chromosphere - Part One - Menzel Coefficients
Authors: Pavlenko, Y. V.
1988Afz....28..163P    Altcode:
  Results of a solution of the NLTE problem for magnesium in the
  atmosphere of a red giant M2 (T<SUB>eff</SUB> = 3800K, log g = 1.5) are
  discussed. An empirical model chromosphere was used. The over-ionization
  of magnesium in the atmosphere of the M2 giant takes place only in
  the region of the temperature minimum. In contrast, the number of
  Mg<SUP>+</SUP> ions in the chromosphere decreased compared with LTE.

---------------------------------------------------------
Title: The Over Ionization of Metals in Atmospheres of M Giants
Authors: Pavlenko, Y. V.
1983ATsir1267....6P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Curve of Growth and Radiation Diffusion in the Case of
    a Hydrogen Multilevel Atom in Prominences
Authors: Yakovkin, N. A.; Zeldina, M. Y.; Pavlenko, Y. V.
1980BSolD..12...89Y    Altcode:
  No abstract at ADS

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Title: Diffusion of Hydrogen Radiation in Prominences
Authors: Yakovkin, N. A.; Zeldina, M. Y.; Pavlenko, Y. V.
1979SvA....23..585Y    Altcode:
  No abstract at ADS