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arXiv:0905.4282
Date: Tue, 26 May 2009 20:00:06 GMT   (154kb,D)

Title: Electron and Gamma Background in CRESST Detectors
Authors: R. F. Lang, G. Angloher, M. Bauer, I. Bavykina, A. Bento, A. Brown, C.
  Bucci, C. Ciemniak, C. Coppi, G. Deuter, F. von Feilitzsch, D. Hauff, S.
  Henry, P. Huff, J. Imber, S. Ingleby, C. Isaila, J. Jochum, M. Kiefer, M.
  Kimmerle, H. Kraus, J.-C. Lanfranchi, B. Majorovits, M. Malek, R. McGowan, V.
  B. Mikhailik, E. Pantic, F. Petricca, S. Pfister, W. Potzel, F. Pr\"obst, S.
  Roth, K. Rottler, C. Sailer, K. Sch\"affner, J. Schmaler, S. Scholl, W.
  Seidel, L. Stodolsky, A. J. B. Tolhurst, I. Usherov, W. Westphal
Categories: astro-ph.IM
Comments: 7 pages, 12 figures
\\
  The CRESST experiment monitors 300g CaWO_4 crystals as targets for particle
interactions in an ultra low background environment. In this paper, we analyze
the background spectra that are recorded by three detectors over many weeks of
data taking. Understanding these spectra is mandatory if one wants to further
reduce the background level, and allows us to cross-check the calibration of
the detectors. We identify a variety of sources, such as intrinsic
contaminations due to primordial radioisotopes and cosmogenic activation of the
target material. In particular, we detect a 3.6keV X-ray line from the decay of
41-Ca with an activity of (26\pm4)\mu Bq, corresponding to a ratio
41-Ca/40-Ca=(2.2\pm0.3)\times10^{-16}.
\\ ( http://arxiv.org/abs/0905.4282 ,  154kb)
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arXiv:0905.4283
Date: Tue, 26 May 2009 20:02:02 GMT   (126kb)

Title: Revisiting the Role of M31 in the Dynamical History of the Magellanic
  Clouds
Authors: Nitya Kallivayalil (MIT), Gurtina Besla (CfA), Robyn Sanderson (MIT),
  Charles Alcock (CfA)
Categories: astro-ph.GA astro-ph.CO
Comments: 10 pages, 5 figures, accepted to ApJ
\\
  We study the dynamics of the Magellanic Clouds in a model for the Local Group
whose mass is constrained using the timing argument/two-body limit of the
action principle. The goal is to evaluate the role of M31 in generating the
high angular momentum orbit of the Clouds, a puzzle that has only been
exacerbated by the latest $HST$ proper motion measurements. We study the
effects of varying the total Local Group mass, the relative mass of the Milky
Way and M31, the proper motion of M31, and the proper motion of the LMC on this
problem. Over a large part of this parameter-space we find that tides from M31
are insignificant. For a range of LMC proper motions approximately $3\sigma$
higher than the mean and total Local Group mass $> 3.5\times 10^{12} M_\odot$,
M31 can provide a significant torque to the LMC orbit. However, if the LMC is
bound to the MW, then M31 is found to have negligible effect on its motion and
the origin of the high angular momentum of the system remains a puzzle.
Finally, we use the timing argument to calculate the total mass of the MW-LMC
system based on the assumption that they are encountering each other for the
first time, their previous perigalacticon being a Hubble time ago, obtaining
$M_{\rm MW} + M_{\rm LMC} = (8.7 \pm 0.8) \times 10^{11} M_\odot$.
\\ ( http://arxiv.org/abs/0905.4283 ,  126kb)
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arXiv:0905.4294
Date: Wed, 27 May 2009 19:11:26 GMT   (592kb)

Title: Feedback from central black holes in elliptical galaxies. II: Can purely
  mechanical energy feedback models work?
Authors: Min-Su Shin (Princeton University), Jeremiah P. Ostriker (Princeton
  University and University of Cambridge), Luca Ciotti (University of Bologna)
Categories: astro-ph.GA
Comments: Submitted to ApJ
\\
  By using high-resolution 1D hydrodynamical simulations, we investigate the
effects of purely mechanical feedback from super massive black holes (SMBHs) in
the evolution of elliptical galaxies for a broad range of feedback efficiencies
and compare the results to four major observational constraints. In particular,
we focus on 1) the central black hole to stellar mass ratio of the host galaxy,
2) the lifetime of the luminous quasar phase, 3) the mass of stars formed in
the host galaxy within the last Gyr, and 4) the X-ray luminosity of the hot
diffuse gas. As a result, we try to pin down the most successful range of
mechanical feedback efficiencies. We find that while low feedback efficiencies
result in too much growth of the SMBH, high efficiencies totally blow out the
hot interstellar gas, and the models are characterized by very low thermal
X-ray luminosity well below the observed range. The net lifetime of the quasar
phase is strongly coupled to the mass ratio between SMBH and its host galaxy,
while the X-ray luminosity is generally correlated to the recent star formation
within the last Gyr. When considering the popularly adopted model of the
constant feedback efficiency, the feedback energy deposited into the ambient
medium should be more than 0.01% of the SMBH accretion energy to be consistent
with the SMBH mass to stellar mass ratio in the local universe. Yet, the X-ray
luminosity of the hot gas favors about 0.005% of the accretion energy as the
mechanical AGN feedback energy. We conclude that the purely mechanical feedback
mode is unlikely to be simultaneously compatible with all four observable
tests, even allowing a broad range of feedback efficiencies, and that including
both radiative and mechanical feedback together may be a solution to comply the
observational constraints. [abridged]
\\ ( http://arxiv.org/abs/0905.4294 ,  592kb)
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arXiv:0905.4297
Date: Tue, 26 May 2009 23:51:46 GMT   (1583kb)

Title: Spatial variations of dust abundances across the Large Magellanic Cloud
Authors: Deborah Paradis, William T. Reach, Jean-Philippe Bernard, Miwa Block,
  Chad W. Engelbracht, Karl Gordon, Joseph L. Hora, Remy Indebetouw, Akiko
  Kawamura, Marilyn Meade, Margaret Meixner, Marta Sewilo, Uma P. Vijh, Kevin
  Volk
Categories: astro-ph.GA
Comments: Received 2009 February 13 ; Accepted 2009 April 28
DOI: 10.1088/0004-6256/137/1/1
\\
  Using the data obtained with the Spitzer Space telescope as part of the
Surveying the Agents of a Galaxy's Evolution (SAGE) legacy survey, we have
studied the variations of the dust composition and abundance across the Large
Magellanic Cloud (LMC). Such variations are expected, as the explosive events
which have lead to the formation of the many HI shells observed should have
affected the dust properties. Using a model and comparing with a reference
spectral energy distribution from our Galaxy, we deduce the relative abundance
variations of small dust grains across the LMC. We examined the infrared color
ratios as well as the relative abundances of very small grains (VSGs) and
polycyclic aromatic hydrocarbons (PAHs) relative to the big grain (BG)
abundance. Results show that each dust component could have different origins
or evolution in the interstellar medium (ISM). The VSG abundance traces the
star formation activity and could result from shattering of larger grains,
whereas the PAH abundance increases around molecular clouds as well as in the
stellar bar, where they could have been injected into the ISM during mass loss
from old stars.
\\ ( http://arxiv.org/abs/0905.4297 ,  1583kb)
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arXiv:0905.4298
Date: Tue, 26 May 2009 22:06:20 GMT   (1169kb)

Title: ChaMPlane Deep Galactic Bulge Survey. I. Faint accretion-driven binaries
  in the Limiting Window
Authors: Maureen van den Berg (CfA), JaeSub Hong (CfA), Jonathan E. Grindlay
  (CfA)
Categories: astro-ph.HE
Comments: 14 pages, 8 figures, 5 tables; accepted for publication in ApJ
\\
  [Abridged] We have carried out a deep X-ray and optical survey with Chandra
and HST of low-extinction regions in the Galactic bulge. Here we present the
results of a search for low-luminosity (L_X <~ 1e34 ergs/s) accreting binaries
in the region closest to the Galactic Center, at an angular offset of 1.4deg,
that we have named the Limiting Window. Based on their blue optical colors,
excess Halpha fluxes, and high X-ray--to--optical flux ratios, we identify
three likely cataclysmic variables (CVs). Distance estimates put these systems
farther than >~2 kpc. Based on their Halpha-excess fluxes and/or high
X-ray--to--optical flux ratios, we find 22 candidate accreting binaries;
however, the properties of some can also be explained if they are dMe stars or
active galaxies. We investigate the CV number density towards the bulge and
find that the number of observed candidate CVs is consistent with or lower than
the number expected for a constant CV-to-star ratio that is fixed to the local
value. The X-ray properties of two likely CVs are similar to those of the
faint, hard X-ray sources in the Galactic-Center region that have been
explained by (mainly) magnetic CVs. If our candidates belong to the same
population, they would be the first members to be optically identified; optical
or infrared identification of their Galactic-Center analogs would be impossible
due to the higher obscuration. We speculate that all Galactic hard X-ray
sources in our field can be explained by magnetic CVs.
\\ ( http://arxiv.org/abs/0905.4298 ,  1169kb)
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arXiv:0905.4300
Date: Tue, 26 May 2009 22:42:40 GMT   (42kb)

Title: NGC7538 IRS1 - an ionized jet powered by accretion
Authors: G. Sandell, W. M. Goss, M. Wright, S. Corder
Categories: astro-ph.SR
Comments: Accepted for Astrophysical Journal Letters
\\
  Analysis of high spatial resolution VLA images shows that the free-free
emission from NGC7538 IRS1 is dominated by a collimated ionized wind. We have
re-analyzed high angular resolution VLA archive data from 6 cm to 7 mm, and
measured separately the flux density from the compact bipolar core and the
extended (1.5" - 3") lobes. We find that the flux density of the core is
proportional to the frequency to the power of alpha, with alpha being about
0.7. The frequency dependence of the total flux density is slightly steeper
with alpha = 0.8. A massive optically thick hypercompact core with a steep
density gradient can explain this frequency dependence, but it cannot explain
the extremely broad recombination line velocities observed in this source.
Neither can it explain why the core is bipolar rather than spherical, nor the
observed decrease of 4% in the flux density in less than 10 years. An ionized
wind modulated by accretion is expected to vary, because the accretion flow
from the surrounding cloud will vary over time. BIMA and CARMA continuum
observations at 3 mm show that the free-free emission still dominates at 3 mm.
HCO+ J = 1 - 0 observations combined with FCRAO single dish data show a clear
inverse P Cygni profile towards IRS1. These observations confirm that IRS1 is
heavily accreting with an accretion rate of about 2 times 10(-4) solar masses
per year.
\\ ( http://arxiv.org/abs/0905.4300 ,  42kb)
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arXiv:0905.4301
Date: Wed, 27 May 2009 18:12:38 GMT   (242kb)

Title: BOOMERanG Constraints on Primordial Non-Gaussianity from Analytical
  Minkowski Functionals
Authors: P. Natoli, G. De Troia, C. Hikage, E. Komatsu, M. Migliaccio, P. A. R.
  Ade, J. J. Bock, J. R. Bond, J. Borrill, A. Boscaleri, C. R. Contaldi, B. P.
  Crill, P. de Bernardis, G. de Gasperis, A. de Oliveira-Costa, G. Di Stefano,
  E. Hivon, T. S. Kisner, W. C. Jones, A. E. Lange, S. Masi, P. D. Mauskopf, C.
  J. MacTavish, A. Melchiorri, T. E. Montroy, C. B. Netterfield, E. Pascale, F.
  Piacentini, G. Polenta, S. Ricciardi, G. Romeo, J. E. Ruhl, M. Tegmark, M.
  Veneziani, N. Vittorio
Categories: astro-ph.CO
Comments: 8 pages, 3 figures
\\
  We use Minkowski Functionals (MF) to constrain a primordial non-Gaussian
contribution to the CMB intensity field as observed in the 150 GHz and 145 GHz
BOOMERanG maps from the 1998 and 2003 flights, respectively, performing for the
first time a joint analysis of the two datasets. A perturbative expansion of
the MF formulae in the limit of a weakly non-Gaussian field yields analytical
formulae, derived by Hikage et al. (2006), which can be used to constrain the
coupling parameter f_NL without the need for non-Gaussian simulations. We find
-1020<f_NL<390 at 95% CL, significantly improving the previous constraints by
De Troia et al. (2007) on the BOOMERanG 2003 dataset. These are the best f_NL
limits to date for suborbital probes.
\\ ( http://arxiv.org/abs/0905.4301 ,  242kb)
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arXiv:0905.4309
Date: Wed, 27 May 2009 01:19:31 GMT   (435kb)

Title: A Revisit of the Masuda Flare
Authors: Rui Liu, Yan Xu, and Haimin Wang
Categories: astro-ph.SR
\\
  We revisit the flare on 1992 January 13, which is now universally termed the
``Masuda flare''. Our work is motivated by the remarkable improvement of Yohkoh
hard X-ray imaging, which was only achieved after the intensive investigations
on this famous event. With the calibrated Hard X-ray Telescope (HXT) data, we
find that the hard X-ray coronal source is indeed a loop-top source, located
slightly above the soft X-ray loop but within the 10% brightness contour of the
HXT L-band thermal loop, rather than distinctly above the loop top as in the
original HXT images. This critical change relieves the longstanding
difficulties of understanding the original Masuda flare, viz., the lack of
L-band emission of the coronal source, and the low density at the coronal
source location. Despite the generally accepted belief that the coronal
emission in the Masuda flare was nonthermal, we find its spectrum can be
explained either by thermal bremsstrahlung of a superhot plasma (80 MK), or by
nonthermal bremsstrahlung at a thick-thin target, with the injecting electron
index derived from the coronal emission approximately equal to that from the
footpoints. We propose a simplified picture, featuring the field line shrinkage
effect and the resultant increase of the loss-cone angle at the coronal trap,
to qualitatively explain that as time progresses the hard X-ray coronal source
diminishes in brightness relative to the footpoints, that its centroid position
moves to higher altitudes, and that the footpoint spectrum is successively
hardening, with the coronal spectrum softening simultaneously.
\\ ( http://arxiv.org/abs/0905.4309 ,  435kb)
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arXiv:0905.4311
Date: Wed, 27 May 2009 01:24:42 GMT   (431kb)

Title: Forecasts for Dark Energy Measurements with Future HI Surveys
Authors: Filipe B. Abdalla, Chris Blake, Steve Rawlings
Categories: astro-ph.CO
Comments: 19 pages; 2 tables; 18 figures. submitted to MNRAS
\\
  We use two independent methods to forecast the dark energy measurements
achievable by combining future galaxy redshift surveys based on the radio HI
emission line with Cosmic Microwave Background (CMB) data from the {\sl Planck}
satellite. In the first method we focus on the `standard ruler' provided by the
baryon acoustic oscillation (BAO) length scale. In the second method we utilize
additional information encoded in the galaxy power spectrum including galaxy
bias from velocity-space distortions and the growth of cosmic structure. We
find that a radio synthesis array with about 10 per cent of the collecting area
of the Square Kilometre Array (SKA), equipped with a wide ($10-100 ~ {\rm
deg}^2$) field-of-view, would have the capacity to perform a $20{,}000 ~ {\rm
deg}^2$ redshift survey to a maximum redshift $z_{\rm max} \sim 0.8$ and
thereby produce dark energy measurements that are competitive with surveys
likely to be undertaken by optical telescopes around 2015. There would then be
powerful arguments for adding collecting area to such a `Phase-1' SKA because
of the square-law scaling of survey speed with telescope sensitivity for HI
surveys, compared to the linear scaling for optical redshift surveys. The full
SKA telescope should, by performing a $20{,}000 ~ {\rm deg}^2$ HI redshift
survey to $z_{\rm max} \sim 2$ around 2020, yield an accurate measurement of
cosmological parameters independent of CMB datasets. Combining CMB ({\sl
Planck}) and galaxy power spectrum (SKA) measurements will drive errors in the
dark energy equation-of-state parameter $w$ well below the 1 per cent level.
The major systematic uncertainty in these forecasts is the lack of direct
information about the mass function of high-redshift HI-emitting galaxies.
\\ ( http://arxiv.org/abs/0905.4311 ,  431kb)
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\\
arXiv:0905.4335
Date: Wed, 27 May 2009 05:11:02 GMT   (38kb)

Title: Curvature, Phase Space, Holography and Black Hole Entropy
Authors: C Sivaram (1) and Kenath Arun (2) ((1) Indian Institute of
  Astrophysics, Bangalore; (2) Christ Junior College, Bangalore)
Categories: astro-ph.CO
Comments: Essay written for the Gravity Research Foundation 2009 Awards for
  Essays on Gravitation; This paper received the Honourable Mention for 2009
  Awards for Essays on Gravitation; 17 equations, 7 pages
\\
  This paper discusses the thermodynamics of a black hole with respect to
Hawking radiation and the entropy. We look at a unified picture of black hole
entropy and curvature and how this can lead to the usual black hole luminosity
due to Hawking radiation. It is also shown how the volume inside the horizon,
apart from surface area, can play a role in understanding the Hawking flux. In
addition holography also implies a phase space associated with the interior
volume and this happens to be just a quantum of phase space, filled with just
one photon. Generalised uncertainty principle can be incorporated in this
analysis. These results hold for all black hole masses in any dimensions.
\\ ( http://arxiv.org/abs/0905.4335 ,  38kb)
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arXiv:0905.4337
Date: Wed, 27 May 2009 05:51:41 GMT   (1518kb)

Title: Variable Stars in the Field of the Open Cluster NGC 2126
Authors: Shun-Fang Liu, Zhen-Yu Wu, Xiao-Bin Zhang, Jiang-Hua Wu, Jun Ma,
  Zhao-Ji Jiang, Jian-Sheng Chen and Xu Zhou
Categories: astro-ph.SR
Comments: 12 pages, accepted for publication in RAA
\\
  We report the results of a time-series CCD photometric survey of variable
stars in the field of the open cluster NGC 2126. In about one square degree
field covering the cluster, a total number of 21 variable candidates are
detected during this survey, of which 16 are newly found. The periods,
classifications and spectral types of 14 newly discovered variables are
discussed, which consist of six eclipsing binaries systems, three pulsating
variable stars, three long period variables, one RS CVn star, and one W UMa or
$\delta$ Scuti star. In addition, there are two variable candidates, the
properties of which cannot be determined in this paper. By a method based on
fitting spectral energy distributions(SEDs) of stars with theoretical ones, the
membership probabilities and the fundamental parameters of this cluster are
determined. As a result, five variables are probably members of NGC 2126. The
fundamental parameters of the this cluster are determined as: the metallicity
to be 0.008 $Z_\odot$, the age $\log(t)$= 8.95, the distance modulus
$(m-M)_{0}$= 10.34 and the reddening value $E(B-V)$=0.55 mag.
\\ ( http://arxiv.org/abs/0905.4337 ,  1518kb)
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arXiv:0905.4344
Date: Wed, 27 May 2009 07:11:18 GMT   (140kb)

Title: Analysis of the spectral energy distribution of the coolest RCrB type
  carbon star DY Per
Authors: L.A.Yakovina (MAO), A.V.Shavrina (MAO), Ya.V.Pavlenko (MAO),
  A.F.Pugach (MAO)
Categories: astro-ph.SR
Comments: 4 pages, 2 tables, 3 figs, accepted by Odessa asronomical observatory
  Publ., 2009
\\
  We analyse the spectral energy distribution of the evolved carbon giant DY
Per with a spectral synthesis technique. The red giant shows the photometric
features of R CrB type stars. We derive the atmospheric parameters of DY Per
using three variants of molecular line lists. We estimate Teff to be in the
range 2900 < Teff < 3300 K. We adopted log g = 0. The star may be metal
deficient and hydrogen deficient. The maximum possible carbon abundance in the
star, [C]=0.94, provides the following atmospheric parameters: Tef=3100 K,
[Fe/H] = 0, log(C/O)=0.6, [N/Fe] = 0, [H/He] = 0, with Jorgensen's line lists
for the molecules C2 and CN.
\\ ( http://arxiv.org/abs/0905.4344 ,  140kb)
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arXiv:0905.4350
Date: Wed, 27 May 2009 07:34:02 GMT   (1436kb)

Title: Could the Galactic disk heating be due to Globular Cluster impacts?
Authors: D. Vande Putte, Mark Cropper, Ignacio Ferreras
Categories: astro-ph.GA
Comments: 4 pages, 1 figure, accepted for publication in MNRAS on 2009/May/14
\\
  So far, six mechanisms have been proposed to account for the Galactic disk
heating. Of these, the most important appear to be a combination of scattering
of stars by molecular clouds and by spiral arms. We study a further mechanism,
namely, the repeated disk impact of the original Galactic Globular Cluster
population up to the present. We find that Globular Clusters could have
contributed at most a small fraction of the current vertical energy of the
disk, as they could heat the whole disk to {$\sigma $}$_{z}$ = 5.5kms$^{{\rm -}
{\rm 1}}$ (c.f. the observed 18 and 39 kms$^{{\rm -} {\rm 1}}$ for the thick
and thin disks respectively). We find that the rate of rise of disk heat
($\alpha$=0.22 in \textit{$\sigma $}$_{z}$ $\sim t^{\alpha}$ with \textit t
being time), is close to that found for scattering by molecular clouds.
\\ ( http://arxiv.org/abs/0905.4350 ,  1436kb)
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arXiv:0905.4354
Date: Wed, 27 May 2009 08:16:18 GMT   (31kb)

Title: O and Na abundance patterns in open clusters of the Galactic disk
Authors: G.M. De Silva, B.K. Gibson, J. Lattanzio, M. Asplund
Categories: astro-ph.GA astro-ph.SR
Comments: To appear in Astronomy and Astrophysics Letters
DOI: 10.1051/0004-6361/200912279
\\
  Aims. A global O-Na abundance anti-correlation is observed in globular
clusters, which is not present in the Galactic field population. Open clusters
are thought to be chemically homogeneous internally. We aim to explore the O
and Na abundance pattern among the open cluster population of the Galactic
disk.
  Methods. We combine open cluster abundance ratios of O and Na from
high-resolution spectroscopic studies in the literature and normalize them to a
common solar scale. We compare the open cluster abundances against the globular
clusters and disk field.
  Results. We find that the different environments show different abundance
patterns. The open clusters do not show the O-Na anti-correlation at the
extreme O-depletion / Na-enhancement as observed in globular clusters.
Furthermore, the high Na abundances in open clusters do not match the disk
field stars. If real, it may be suggesting that the dissolution of present-day
open clusters is not a significant contribution to building the Galactic disk.
Large-scale homogeneous studies of clusters and field will further confirm the
reality of the Na enhancement.
\\ ( http://arxiv.org/abs/0905.4354 ,  31kb)
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\\
arXiv:0905.4357
Date: Wed, 27 May 2009 09:00:26 GMT   (698kb)

Title: Similarity between the Molecular Loops in the Galactic Center and the
  Solar Chromospheric Arch Filaments
Authors: Kunio Takahashi (1), Satoshi Nozawa (2), Ryoji Matsumoto (3), Mami
  Machida (1), Yasuo Fukui (4), Natsuko Kudo (4), Kazufumi Torii (4), Hiroaki
  Yamamoto (4), and Motosuji Fujishita (4) ((1)National Astronomical
  Observatory of Japan,(2)Ibaraki University,(3)Chiba University,(4)Nagoya
  University)
Categories: astro-ph.SR
Comments: 23 pages, 13 figures. Accepted for publication in PASJ
\\
  We carried out two-dimensional magnetohydrodynamic simulations of the
Galactic gas disk to show that the dense loop-like structures discovered by the
Galactic center molecular cloud survey by NANTEN 4 m telescope can be formed by
the buoyant rise of magnetic loops due to the Parker instability. At the
initial state, we assumed a gravitationally stratified disk consisting of the
cool layer ($T \sim 10^3$ K), warm layer ($T \sim 10^4$ K), and hot layer ($T
\sim 10^5$ K). Simulation box is a local part of the disk containing the
equatorial plane. The gravitational field is approximated by that of a point
mass at the galactic center. The self-gravity, and the effects of the galactic
rotation are ignored. Numerical results indicate that the length of the
magnetic loops emerging from the disk is determined by the scale height of the
hot layer ($\sim$ 100 pc at 1 kpc from the Galactic center). The loop length,
velocity gradient along the loops and large velocity dispersions at their foot
points are consistent with the NANTEN observations. We also show that the loops
become top-heavy when the curvature of the loop is sufficiently small, so that
the rising loop accumulates the overlying gas faster than sliding it down along
the loop. This mechanism is similar to that of the formation of solar
chromospheric arch filaments. The molecular loops emerge from the low
temperature layer just like the dark filaments observed in the H$\alpha$ image
of the emerging flux region of the sun.
\\ ( http://arxiv.org/abs/0905.4357 ,  698kb)
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arXiv:0905.4361
Date: Wed, 27 May 2009 09:00:09 GMT   (476kb)

Title: Clustering of K-band selected local galaxies
Authors: Bin Ma, Kelai Meng, Jun Pan, Jiasheng Huang, Longlong Feng
Categories: astro-ph.CO
Comments: 13 pages, 6 figures, accepted by RAA
\\
  We present detailed clustering analysis of a large K-band selected local
galaxy sample, which is constructed from the 2MASS and the SDSS and consists of
$82,486$ galaxies with $10 < K < 13.5$ and $0.01 < z < 0.1$. The two-point
correlation function of the magnitude-limited sample in real space at small
scales is well described by a power law
$\xi(r)=(r/6.44\pm0.23)^{-1.81\pm0.02}$. The pairwise velocity dispersion is
derived from the anisotropic two-point correlation function and find the
dispersion $\sigma_{12}=685\pm 17\kms$ if its scale invariance is assumed,
which is larger than values measured in optical bands selected galaxy samples.
We further investigate the dependence of the two-point correlation function and
the $\sigma_{12}$ on the $g-r$ color and the $K$-band luminosity, obtain
similar results to previous works in optical bands. Comparing a mock galaxy
sample with our real data indicates that the semi-analytical model can not
mimic the $\sigma_{12}$ in observation albeit it can approximate the two-point
correlation function within measurement uncertainties.
\\ ( http://arxiv.org/abs/0905.4361 ,  476kb)
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arXiv:0905.4364
Date: Wed, 27 May 2009 09:36:17 GMT   (246kb)

Title: Complexity and neutron stars structure
Authors: K.Ch. Chatzisavvas, V.P. Psonis, C.P. Panos, Ch.C. Moustakidis
Categories: astro-ph.SR quant-ph
Comments: Preprint, 23 pages, 28 figures
\\
  We apply the statistical measure of complexity introduced by Lopez-Ruiz,
Mancini and Calbet to neutron stars structure. Neutron stars is a classical
example where the gravitational field and quantum behavior are combined and
produce a macroscopic dense object. Actually, we continue the recent
application of Sanudo and Pacheco to white dwarfs structure. We concentrate our
study on the connection between complexity and neutron star properties, like
maximum mass and the corresponding radius, applying a specific set of realistic
equation of states. Moreover, the effect of the strength of the gravitational
field on the neutron star structure and consequently on the complexity measure
is also investigated. It is seen that neutron stars, consistent with
astronomical observations so far, are ordered systems (low complexity), which
cannot grow in complexity as their mass increases. This is a result of the
interplay of gravity, the short-range nuclear force and the very short-range
weak interaction.
\\ ( http://arxiv.org/abs/0905.4364 ,  246kb)
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arXiv:0905.4365
Date: Wed, 27 May 2009 09:40:20 GMT   (249kb)

Title: Nucleosynthesis of light element isotopes in evolved stars experiencing
  extended mixing
Authors: S. Palmerini, M. Busso, E. Maiorca and R. Guandalini
Categories: astro-ph.SR
Comments: 8 pages, 7 figures, proceeding of 'The Origin of the Elements Heavier
  than Fe' September 24-28, 2008, Torino, Italy. PASA (accepted for
  publication)
\\
  We present computations of nucleosynthesis in red giants and asymptotic giant
branch stars of Population I experiencing extended mixing. The assumed physical
cause for mass transport is the buoyancy of magnetized structures, according to
recent suggestions. The peculiar property of such a mechanism is to allow for
both fast and slow mixing phenomena, as required for reproducing the spread in
Li abundances displayed by red giants and as discussed in an accompanying
paper. We explore here the effects of this kind of mass transport on CNO and
intermediatemass nuclei and compare the results with the available evidence
from evolved red giants and from the isotopic composition of presolar grains of
AGB origin. It is found that a good general accord exists between predictions
and measurements; in this framework we also show which type of observational
data best constrains the various parameters. We conclude that magnetic
buoyancy, allowing for mixing at rather different speeds, can be an interesting
scenario to explore for explaining together the abundances of CNO nuclei and of
Li.
\\ ( http://arxiv.org/abs/0905.4365 ,  249kb)
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\\
arXiv:0905.4366
Date: Wed, 27 May 2009 09:47:03 GMT   (1930kb)

Title: Suzaku Observation of the Metallicity in the Interstellar Medium of NGC
  4258
Authors: Saori Konami, Kosuke Sato, Kyoko Matsushita, Shin'ya Yamada, Naoki
  Isobe, Atsushi Senda, Asami Hayato, Poshak Gandhi, Toru Tamagawa, Kazuo
  Makishima
Categories: astro-ph.CO
Comments: 9 pages, 4 figures
\\
  The Suzaku X-ray satellite observed the nearby spiral galaxy NGC 4258 for a
total good exposure time of 100 ks. We present an analysis of the Suzaku XIS
data, in which we confirm that the 0.5--2 keV spectra of the interstellar
medium (ISM) are well-represented by a two-temperature model. The cool and hot
ISM temperatures are 0.23+-0.02 and 0.59 +-0.01 keV, respectively. Suzaku's
excellent spectral sensitivity enables us to measure the metal abundances of O,
Ne, Mg, Si and Fe of the ISM for the first time. The resultant abundance
pattern of O, Mg, Si, and Fe is consistent with that of the new solar abundance
table of Lodders (2003), rather than Anders & Grevesse (1989). This suggests
that the metal enrichment processes of NGC 4258 and of our Galaxy are similar.
\\ ( http://arxiv.org/abs/0905.4366 ,  1930kb)
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\\
arXiv:0905.4383
Date: Wed, 27 May 2009 11:35:31 GMT   (162kb)

Title: The detection of Broad Iron K and L line emission in the Narrow-Line
  Seyfert 1 Galaxy 1H0707-495 using XMM-Newton
Authors: A.C. Fabian, A. Zoghbi, R.R. Ross, P. Uttley, L.C. Gallo, W.N. Brandt,
  A. Blustin, T. Boller, M.D. Caballero-Garcia, J. Larsson, J.M. Miller, G.
  Miniutti, G. Ponti, R.C. Reis, C.S. Reynolds, Y. Tanaka, A.J. Young
Categories: astro-ph.HE astro-ph.CO
Comments: To appear in Nature May 28 2009, 12 pages with 11 figures
\\
  Since the discovery of the first broad iron-K line in 1995 from the Seyfert
Galaxy MCG--6-30-15, broad iron-K lines have been found in several other
Seyfert galaxies, from accreting stellar mass black holes and even from
accreting neutron stars. The iron-K line is prominent in the reflection
spectrum created by the hard X-ray continuum irradiating dense accreting
matter. Relativistic distortion of the line makes it sensitive to the strong
gravity and spin of the black hole. The accompanying iron-L line emission
should be detectable when the iron abundance is high. Here we report the first
discovery of both iron-K and L emission, using XMM-Newton observations of the
Narrow-Line Seyfert 1 Galaxy 1H0707-495. The bright Fe-L emission has enabled
us, for the first time, to detect a reverberation lag of 30 s between the
direct X-ray continuum and its reflection from matter falling into the hole.
The observed reverberation timescale is comparable to the light-crossing time
of the innermost radii around a supermassive black hole. The combination of
spectral and timing data on 1H0707-495 provides strong evidence that we are
witnessing emission from matter within a gravitational radius, or a fraction of
a light-minute, from the event horizon of a rapidly-spinning, massive black
hole.
\\ ( http://arxiv.org/abs/0905.4383 ,  162kb)
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\\
arXiv:0905.4389
Date: Wed, 27 May 2009 11:58:44 GMT   (204kb)

Title: AGN dust tori: the X-ray-infrared connection
Authors: Michael Rowan-Robinson (Imperial College), Ivan Valtchanov (ESAC,
  ESA), Kirpal Nandra (Imperial College)
Categories: astro-ph.CO
Comments: 15 pages, 18 figures, accepted for publication MNRAS
\\
  We have combined the CLASX Chandra survey in Lockman with the Spitzer SWIRE
survey data to study the X-ray-infrared connection for AGN. The sample consists
of 401 X-ray-sources, of which 306 are detected by Spitzer, and a further 257
AGN candidates detected through their dust torus, but not by Chandra. For X-ray
sources the X-ray hardness ratio has been modelled in terms of a power-law with
absorption N(H). The optical and infrared data have been modelled in terms of
our well-established optical galaxy and QSO templates, and infrared templates
based on radiative transfer models.
  Our estimate of the N(H) distribution is consistent with other studies, but
we do find a higher proportion of low absorption objects at z < 0.5 than at z >
0.5. While we find only one X-ray AGN with N(H) > 10^{24} cm^{-2}, we argue
that 10 objects with torus luminosity apparently exceeding the bolometric X-ray
to 3 \mu m luminosity are strong candidates for being heavily absorbed in
X-rays. We also estimate that at least half of the infrared-detected AGN dust
tori which are undetected in X-rays are likely to be Compton thick. Our
estimate of the total number of Compton-thick objects corresponds to > 20%$ of
the combined SWIRE-CLASX sample (and with an upper limit of 39 %).
  The range of dust covering factors is 1-100 %, with a mean of 40 %, ie a Type
2 fraction of 40 %. Measured by the ratio of dust torus luminosity to X-ray or
(for Type 1 objects) optical luminosity, the covering factor appears to
decrease towards intermediate AGN luminosity, in contradiction to estimates
based on ratios of narrow-line and broad-line spectra, but may increase again
at low AGN luminosity.
\\ ( http://arxiv.org/abs/0905.4389 ,  204kb)
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\\
arXiv:0905.4400
Date: Wed, 27 May 2009 12:32:51 GMT   (290kb)

Title: Pulsed Gamma-rays from PSR J2021+3651 with the Fermi Large Area
  Telescope
Authors: A.A.Abdo, et al. (Fermi LAT collaboration and Fermi Pulsar Timing
  Consortium)
Categories: astro-ph.HE astro-ph.GA
Comments: Accepted by the Astrophysical Journal, 25 May 2009
\\
  We report the detection of pulsed gamma-rays from the young, spin-powered
radio pulsar PSR J2021+3651 using data acquired with the Large Area Telescope
(LAT) on the Fermi Gamma-ray Space Telescope (formerly GLAST). The light curve
consists of two narrow peaks of similar amplitude separated by 0.468 +/- 0.002
in phase. The first peak lags the maximum of the 2 GHz radio pulse by 0.162 +/-
0.004 +/- 0.01 in phase. The integral gamma-ray photon flux above 100 MeV is
(56 +/- 3 +/- 11) x 10^{-8} /cm2/s. The photon spectrum is well-described by an
exponentially cut-off power law of the form dF/dE = kE^{-\Gamma} e^(-E/E_c)
where the energy E is expressed in GeV. The photon index is \Gamma = 1.5 +/-
0.1 +/- 0.1 and the exponential cut-off is E_c = 2.4 +/- 0.3 +/- 0.5 GeV. The
first uncertainty is statistical and the second is systematic. The integral
photon flux of the bridge is approximately 10% of the pulsed emission, and the
upper limit on off-pulse gamma-ray emission from a putative pulsar wind nebula
is <10% of the pulsed emission at the 95% confidence level. Radio polarization
measurements yield a rotation measure of RM = 524 +/- 4 rad/m^2 but a poorly
constrained magnetic geometry. Re-analysis of Chandra data enhanced the
significance of the weak X-ray pulsations, and the first peak is roughly
phase-aligned with the first gamma-ray peak. We discuss the emission region and
beaming geometry based on the shape and spectrum of the gamma-ray light curve
combined with radio and X-ray measurements, and the implications for the pulsar
distance. Gamma-ray emission from the polar cap region seems unlikely for this
pulsar.
\\ ( http://arxiv.org/abs/0905.4400 ,  290kb)
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\\
arXiv:0905.4404
Date: Wed, 27 May 2009 12:44:16 GMT   (778kb)

Title: Two-fluid Instability of Dust and Gas in the Dust Layer of a
  Protoplanetary Disk
Authors: Naoki Ishitsu, Shu-ichiro, Minoru Sekiya
Categories: astro-ph.EP
Comments: 26pages, 11figures, Submitted to ApJ
\\
  Instabilities of the dust layer in a protoplanetary disk are investigated. It
is known that the streaming instability develops and dust density concentration
occurs in a situation where the initial dust density is uniform. This work
considers the effect of initial dust density gradient vertical to the midplane.
Dust and gas are treated as different fluids. Pressure of dust fluid is assumed
to be zero. The gas friction time is assumed to be constant. Axisymmetric
two-dimensional numerical simulation was performed using the spectral method.
We found that an instability develops with a growth rate on the order of the
Keplerian angular velocity even if the gas friction time multiplied by the
Keplerian angular velocity is as small as 0.001.
  This instability is powered by two sources: (1) the vertical shear of the
azimuthal velocity, and (2) the relative motion of dust and gas coupled with
the dust density fluctuation due to advection. This instability diffuses dust
by turbulent advection and the maximum dust density decreases. This means that
the dust concentration by the streaming instability which is seen in the case
of a uniform initial dust density becomes ineffective as dust density gradient
increases by the dust settling toward the midplane.
\\ ( http://arxiv.org/abs/0905.4404 ,  778kb)
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\\
arXiv:0905.4413
Date: Wed, 27 May 2009 13:12:25 GMT   (149kb)

Title: Extending Big Power Law in the Sky with Turbulence Spectra from WHAM
  data
Authors: A. Chepurnov, A. Lazarian
Categories: astro-ph.GA
\\
  We use the data of Wisconsin H$\alpha$ Mapper (WHAM) to test the hypothesis
of whether the amplitudes and spectrum of density fluctuations measured by WHAM
may be matched to the data obtained for interstellar scintillations and
scattering. To do this, first of all, adjusted the mean level of signal in the
adjacent patches of the data. Then, assuming that the spectrum is Kolmogorov,
we successfully matched the amplitudes of turbulence obtained from the WHAM
data and the interstellar density fluctuations reported in the existing
literature. As a result, we conclude that the existing data is consistent with
the a Kolmogorov cascade which spans from $10^6$ to $10^{17}$ $m$.
\\ ( http://arxiv.org/abs/0905.4413 ,  149kb)
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\\
arXiv:0905.4415
Date: Wed, 27 May 2009 13:22:56 GMT   (594kb)

Title: Synthetic photometry for carbon rich giants, I. Hydrostatic dust-free
  models
Authors: B. Aringer, L. Girardi, W. Nowotny, P. Marigo, M. T. Lederer
Categories: astro-ph.SR
Comments: accepted for publication by Astronomy & Astrophysics, 16 pages, 20
  figures
\\
  We study the spectroscopic and photometric properties of carbon stars. In the
first paper of this series we focus on objects that can be described by
hydrostatic models neglecting dynamical phenomena like pulsation and mass loss.
As a consequence, the reddening due to circumstellar dust is not included. Our
results are collected in a database, which can be used in conjunction with
stellar evolution and population synthesis calculations involving the AGB. We
have computed a grid of 746 spherically symmetric COMARCS atmospheres covering
effective temperatures between 2400 and 4000K, surface gravities from log(g) =
0.0 to -1.0, metallicities ranging from the solar value down to one tenth of it
and C/O ratios in the interval between 1.05 and 5.0. Subsequently, we used
these models to create synthetic low resolution spectra and photometric data
for a large number of filter systems. The tables including the results are
electronically available. We have selected some of the most commonly used
colours in order to discuss their behaviour as a function of the stellar
parameters. A comparison with measured data shows that down to 2800K the
agreement between predictions and observations of carbon stars is good. Below
this limit the synthetic colours are much too blue. The obvious reason for
these problems is the neglect of circumstellar reddening and structural changes
due to pulsation and mass loss.
\\ ( http://arxiv.org/abs/0905.4415 ,  594kb)
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\\
arXiv:0905.4424
Date: Wed, 27 May 2009 13:51:08 GMT   (2715kb)

Title: Probing the 2-D kinematic structure of early-type galaxies out to 3
  effective radii
Authors: Robert N. Proctor, Duncan A. Forbes, Aaron J. Romanowsky, Jean P.
  Brodie, Jay Strader, Max Spolaor, J. Trevor Mendel, Lee Spitler
Categories: astro-ph.GA
Comments: 20 pages, 22 figures, Accepted for publication in MNRAS
\\
  We detail an innovative new technique for measuring the 2-D velocity moments
(rotation velocity, velocity dispersion and Gauss-Hermite coefficients h$_3$
and h$_4$) of the stellar populations of galaxy halos using spectra from Keck
DEIMOS multi-object spectroscopic observations. The data are used to
reconstruct 2-D rotation velocity maps.
  Here we present data for five nearby early-type galaxies to ~3 effective
radii. We provide significant insights into the global kinematic structure of
these galaxies, and challenge the accepted morphological classification in
several cases. We show that between 1-3 effective radii the velocity dispersion
declines very slowly, if at all, in all five galaxies. For the two galaxies
with velocity dispersion profiles available from planetary nebulae data we find
very good agreement with our stellar profiles. We find a variety of rotation
profiles beyond 1 effective radius, i.e rotation speed remaining constant,
decreasing \emph{and} increasing with radius. These results are of particular
importance to studies which attempt to classify galaxies by their kinematic
structure within one effective radius, such as the recent definition of fast-
and slow- rotator classes by the SAURON project. Our data suggests that the
rotator class may change when larger galacto-centric radii are probed. This has
important implications for dynamical modeling of early-type galaxies. The data
from this study are available on-line.
\\ ( http://arxiv.org/abs/0905.4424 ,  2715kb)
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\\
arXiv:0905.4431
Date: Wed, 27 May 2009 14:18:11 GMT   (226kb)

Title: Fast optical variability of Naked-Eye Burst - manifestation of periodic
  activity of internal engine
Authors: G. Beskin, S. Karpov, S. Bondar, A. Guarnieri, C. Bartolini, G. Greco,
  A. Piccioni
Categories: astro-ph.HE
Comments: Submitted to Science; please note that this manuscript is subject to
  press embargo
\\
  We imaged the position of the Naked-Eye Burst, GRB080319B, before, during and
after its gamma-ray activity with sub-second temporal resolution and discovered
the fast variability of its prompt optical emission. Its characteristics and
similarity with properties of gamma emission temporal structure suggest that it
reflects the behaviour of internal engine -- supposedly, a hyperaccreting
solar-mass black hole formed in the collapse of a massive stellar core.
\\ ( http://arxiv.org/abs/0905.4431 ,  226kb)
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\\
arXiv:0905.4432
Date: Wed, 27 May 2009 14:13:26 GMT   (2509kb)

Title: The Science Case for PILOT I: Summary and Overview
Authors: J.S. Lawrence, M.C.B. Ashley, J. Bailey, D. Barrado y Navascues, T.
  Bedding, J. Bland-Hawthorn, I. Bond, F. Boulanger, R. Bouwens, H. Bruntt, A.
  Bunker, D. Burgarella, M.G. Burton, M. Busso, D. Coward, M.-R. Cioni, G.
  Durand, C. Eiroa, N. Epchtein, N. Gehrels, P. Gillingham, K. Glazebrook, R.
  Haynes, L. Kiss, P.O. Lagage, T. Le Bertre, C. Mackay, J.P. Maillard, A.
  McGrath, V. Minier, A. Mora, K. Olsen, P. Persi, K. Pimbblet, R. Quimby, W.
  Saunders, B. Schmidt, D. Stello, J.W.V. Storey, C. Tinney, P. Tremblin, J.C.
  Wheeler, P. Yoc
Categories: astro-ph.IM
Comments: 19 pages, 8 figures, accepted for publication in PASA
\\
  PILOT (the Pathfinder for an International Large Optical Telescope) is a
proposed 2.5 m optical/infrared telescope to be located at Dome C on the
Antarctic plateau. Conditions at Dome C are known to be exceptional for
astronomy. The seeing (above ~30 m height), coherence time, and isoplanatic
angle are all twice s good as at typical mid-latitude sites, while the
water-vapour column, and the atmosphere and telescope thermal emission are all
an order of magnitude better. These conditions enable a unique scientific
capability for PILOT, which is addressed in this series of papers. The current
paper presents an overview of the optical and instrumentation suite for PILO
and its expected performance, a summary of the key science goals and
observational approach for the facility, a discussion of the synergies between
the science goals for PILOT and other telescopes, and a discussion of the
future of Antarctic astronomy. Paper II and Paper III present details of the
science projects divided, respectively, between the distant Universe (i.e.,
studies of first light, and the assembly and evolution of structure) and the
nearby Universe (i.e., studies of Local Group galaxies, the Milky Way, and the
Solar System).
\\ ( http://arxiv.org/abs/0905.4432 ,  2509kb)
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\\
arXiv:0905.4439
Date: Wed, 27 May 2009 15:11:19 GMT   (39kb)

Title: The bolometric luminosity of type 2 AGN from extinction-corrected
  [OIII]: no evidence for Eddington-limited sources
Authors: A. Lamastra, S. Bianchi, G. Matt, G. C. Perola, X. Barcons, F. J.
  Carrera
Categories: astro-ph.CO
Comments: 8 pages, 4 figures, accepted for publication in Astronomy and
  Astrophysics
\\
  There have been recent claims that a significant fraction of type 2 AGN
accrete close or even above the Eddington limit. In type 2 AGN the bolometric
luminosity (L_b) is generally inferred from the [OIII] emission line luminosity
(L_OIII). The key issue, in order to estimate the bolometric luminosity in
these AGN, is therefore to know the bolometric correction to be applied to
L_OIII. A complication arises from the fact that the observed L_OIII is
affected by extinction, likely due to dust within the narrow line region. The
extinction-corrected [OIII] luminosity (L^c_OIII) is a better estimator of the
nuclear luminosity than L_OIII. However, so far only the bolometric correction
to be applied to the uncorrected L_OIII has been evaluated. This paper is
devoted to estimate the bolometric correction C_OIII=L_b/L^c_OIII in order to
derive the Eddington ratios for the type 2 AGN in a sample of SDSS objects. We
have collected from the literature 61 sources with reliable estimate of both
L^c_OIII and X-ray luminosities (L_X). To estimate C_OIII, we combined the
observed correlation between L^c_OIII and L_X with the X-ray bolometric
correction. We found, contrary to previous studies, a linear correlation
between L^c_OIII and L_X. We estimated C_OIII using the luminosity-dependent
X-ray bolometric correction of Marconi et al. (2004), and we found a mean value
of C_OIII in the luminosity ranges log L_OIII=38-40, 40-42, and 42-44 of 87,
142 and 454 respectively. We used it to calculate the Eddington ratio
distribution of type 2 SDSS AGN at 0.3<z<0.4 and we found that these sources
are not accreting near their Eddington limit, contrary to previous claims.
\\ ( http://arxiv.org/abs/0905.4439 ,  39kb)
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\\
arXiv:0905.4440
Date: Wed, 27 May 2009 14:38:28 GMT   (4968kb,D)

Title: Accretion of a massive magnetized torus on a rotating black hole
Authors: Maxim V. Barkov and Anton N. Baushev
Categories: astro-ph.HE
Comments: 11 pages, 9 figures, submitted to MNRAS
\\
  We present numerical simulations of the axisymmetric accretion of a massive
magnetized plasma torus on a rotating black hole. We use a realistic equation
of state, which takes into account neutrino cooling and energy loss due to
nucleus dissociations. We simulated various magnetic field configurations and
torus models, both optically thick and thin for neutrinos. It is shown that the
neutrino cooling does not significantly change either the structure of the
accretion flow or the total energy release of the system. The calculations
evidence heating of the wind surrounding the collapsar by the shock waves
generated at the jet-wind border. This mechanism can give rise to a hot corona
around the binary system like SS433.
  Angular momentum of the accreting matter defines the time scale of the
accretion. Due to the absence of the magnetic dynamo in our calculations, the
initial strength and topology of the magnetic field determines magnetization of
the black hole, jet formation properties and the total energy yield. We
estimated the total energy transformed to jets as $1.3\times 10^{52}$ {ergs}
which was sufficient to explain hypernova explosions like GRB 980425 or GRB
030329.
\\ ( http://arxiv.org/abs/0905.4440 ,  4968kb)
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\\
arXiv:0905.4442
Date: Wed, 27 May 2009 14:40:35 GMT   (1087kb)

Title: Calibration and Interpixel Capacitance of a H2RG(2Kx2K) Near-IR Detector
Authors: G. Smadja, C. Cerna, A. Ealet
Categories: astro-ph.IM
\\
  A temporal analysis of the noise is performed, and non linearities are taken
into account. We then extend the correlation method to groups of several pixels
to derive the interpixel capacitance of a detector, found to be x = -0.0263 +/-
0.0020 (stat) +/- 0.0040 (syst). All measurements are consistent to a
sub-percent accuracy.
\\ ( http://arxiv.org/abs/0905.4442 ,  1087kb)
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\\
arXiv:0905.4458
Date: Wed, 27 May 2009 15:46:17 GMT   (176kb)

Title: Extra-Mixing in Luminous Cool Red Giants. Hints from Evolved Stars with
  and without Li
Authors: R. Guandalini (1), S. Palmerini (1), M. Busso (1), S. Uttenthaler (2)
  ((1) Dipartimento di Fisica, Universita' degli Studi di Perugia and INFN,
  sezione di Perugia, Italy, (2) Instituut voor Sterrenkunde, K. U. Leuven,
  Belgium)
Categories: astro-ph.SR
Comments: 8 pages, 6 figures, accepted for publication in PASA
\\
  We present an analysis of Li abundances in low mass stars (LMS) during the
Red Giant Branch (RGB) and Asymptotic Giant Branch (AGB) stages, based on a new
determination of their luminosities and evolutionary status. By applying
recently suggested models for extra-mixing, induced by magnetic buoyancy, we
show that both Li-rich and Li-poor stars can be accounted for. The simplest
scenario implies the development of fast instabilities on the RGB, where Li is
produced. When the fields increase in strength, buoyancy slows down and Li is
destroyed. 3He is consumed, at variable rates. The process continues on the
AGB, where however moderate mass circulation rates have little effect on Li due
to the short time available. O-rich and C-rich stars show different histories
of Li production/destruction, possibly indicative of different masses. More
complex transport schemes are allowed by magnetic buoyancy, with larger effects
on Li, but most normal LMS seem to show only the range of Li variation
discussed here.
\\ ( http://arxiv.org/abs/0905.4458 ,  176kb)
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\\
arXiv:0905.4460
Date: Wed, 27 May 2009 15:51:19 GMT   (320kb)

Title: A Systematic Search for Corotating Interaction Regions in Apparently
  Single Galactic WR Stars. I. Characterizing the Variability
Authors: N. St-Louis, A.-N. Chene, O. Schnurr, M.-H. Nicol
Categories: astro-ph.SR
Comments: 25 pages, 13 figures
\\
  We present the results of a systematic search for large-scale spectroscopic
variability in apparently single Wolf-Rayet stars brighter than ~12.5. In this
first paper we characterize the various forms of variability detected and
distinguish several separate groups. For each star in our sample, we obtained
4-5 high-resolution spectra with a signal-to-noise ratio ~100. Our ultimate
goal is to identify new candidates presenting variability that potentially
comes from Co-rotating Interaction Regions (CIR).
  Out of a sample of 25 stars, 10 were found to display large-scale changes of
which 4 are of CIR-type (WR1, WR115, WR120 and WR134). The star WR134 was
already known to show such changes from previous studies. Three WN8 stars
present a different type of large-scale variability and we believe deserve a
group of their own. Also, all three WC9d stars in our sample present
large-scale variability, but it remains to be checked if these are binaries, as
many dust-making WR stars are double. Finally, of the remaining stars, 10 were
found to show small-amplitude spectral changes which we attribute to normal
line-profile variability due to inhomogeneities in the wind, and 5 were found
to show no spectral variability, as far as can be concluded from the data in
hand.
  Follow-up studies are required to identify potential periods for our
candidates showing CIR-type changes and eventually estimate a rotation rate for
these WR stars.
\\ ( http://arxiv.org/abs/0905.4460 ,  320kb)
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\\
arXiv:0905.4466
Date: Wed, 27 May 2009 16:16:46 GMT   (122kb)

Title: Ultra high energy cosmic rays: subluminal and superluminal shocks
Authors: A. Meli, J.K. Becker, J.J Quenby
Categories: astro-ph.HE
Comments: 4 pages, 4 figures, paper contribution for the International Cosmic
  Ray Conference 2009, Lodz Poland
\\
  Diffusive shock acceleration is invoked to explain non-thermal particle
acceleration in Supernova Remnants, Active Galactic Nuclei (AGN) Jets, Gamma
ray Bursts (GRBs) and various large scale cosmic structures. The importance of
achieving the highest observed particle energies by such a mechanism in a given
astrophysical situation is a recurring theme. In this work, shock acceleration
in relativistic shocks is discussed, mostly focusing on a numerical study
concerning proton acceleration efficiency by subluminal and superluminal
shocks, emphasising on the dependence of the scattering model, bulk Lorentz
factor and the angle between the magnetic field and the shock flow. We
developed a diffuse cosmic ray model based on the study of different shock
boost factors, which shows that spectra from AGN fit current observations of
ultra high energy cosmic rays, above 5.7 x 10^10 GeV, much better than GRBs,
indicating that AGN are the primary candidates to explain the UHECR flux.
Recent Fermi observations of GRB090816c indicate very flat spectra which are
expected within our model predictions and support evidence that GRB particle
spectra can be flat, when the shock Lorentz factor is of order ~1000.
\\ ( http://arxiv.org/abs/0905.4466 ,  122kb)
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\\
arXiv:0905.4473
Date: Wed, 27 May 2009 16:56:02 GMT   (158kb)

Title: A MIKE + UVES survey of Sub-Damped Lyman-Alpha Systems at z<1.5
Authors: Joseph D. Meiring, James T. Lauroesch, Varsha P. Kulkarni, Celine
  Peroux, Pushpa Khare, Donald G. York
Categories: astro-ph.CO
Comments: 13 Pages, 14 Pages: Accepted for Publication in MNRAS 5/2009
\\
  We have combined the results from our recent observations of Damped and
sub-Damped Lyman-alpha systems with the MIKE and UVES spectrographs on the
Magellan Clay and VLT Kueyen telescopes with ones from the literature to
determine the N(HI)-weighted mean metallicity of these systems based both on
Fe, a depleted element in QSO absorbers and the local ISM, and Zn a relatively
undepleted element. In each case, the N(HI)-weighted mean metallicity is higher
and shows faster evolution in sub-DLAs than the classical DLA systems. Large
grids of photoionisation models over the sub-DLA \nhI range with CLOUDY show
that the ionisation corrections to the abundances are in general small, however
the fraction of ionized H can be up to ~90 per cent. The individual spectra
have been shifted to the rest frame of the absorber and averaged together to
determine the average properties of these systems at z<1.5. We find that the
average abundance pattern of the Sub-DLA systems is similar to the gas in the
halo of the Milky Way, with an offset of ~0.3 dex in the overall metallicity.
Both DLAs and Sub-DLAs show similar characteristics in their relative
abundances patterns, although the DLAs have smaller <[Mn/Zn]> as well as higher
<[Ti/Zn]> and <[Cr/Zn]>. We calculate the contribution of sub-DLAs to the metal
budget of the Universe, and find that the sub-DLA systems at z<1.5 contain a
comoving density of metals Omega_met (3.5-15.8)x10^{5} M_sun Mpc^{-3}, at least
twice the comoving density of metals in the DLA systems. The sub-DLAs do
however track global chemical evolution models much more closely than do the
DLAs, perhaps indicating that they are a less dust biased metallicity indicator
of galaxies at high redshifts than the DLA systems.
\\ ( http://arxiv.org/abs/0905.4473 ,  158kb)
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\\
arXiv:0905.4477
Date: Wed, 27 May 2009 17:18:32 GMT   (489kb)

Title: The effect of rotation on the stability of nuclear burning in accreting
  neutron stars
Authors: L. Keek, N. Langer, J.J.M. in 't Zand
Categories: astro-ph.HE
Comments: 11 pages, 11 figures, accepted for publication in Astronomy and
  Astrophysics
\\
  Hydrogen and/or helium accreted by a neutron star from a binary companion may
undergo thermonuclear fusion. At different mass accretion rates different
burning regimes are discerned. Theoretical models predict helium fusion to
proceed as a thermonuclear runaway for accretion rates below the Eddington
limit and as stable burning above this limit. Observations, however, place the
boundary close to 10% of the Eddington limit. We study the effect of
rotationally induced transport processes on the stability of helium burning.
For the first time detailed calculations of thin helium shell burning on
neutron stars are performed using a hydrodynamic stellar evolution code
including rotation and rotationally induced magnetic fields. We find that in
most cases the instabilities from the magnetic field provide the dominant
contribution to the chemical mixing, while Eddington-Sweet circulations become
important at high rotation rates. As helium is diffused to greater depths, the
stability of the burning is increased, such that the critical accretion rate
for stable helium burning is found to be lower. Combined with a higher heat
flux from the crust, as suggested by recent studies, turbulent mixing could
explain the observed critical accretion rate. Furthermore, close to this
boundary we find oscillatory burning, which previous studies have linked to mHz
QPOs. In models where we continuously lower the heat flux from the crust, the
period of the oscillations increases by up to several tens of percents, similar
to the observed frequency drift, suggesting that this drift could be caused by
the cooling of deeper layers.
\\ ( http://arxiv.org/abs/0905.4477 ,  489kb)
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\\
arXiv:0905.4484
Date: Wed, 27 May 2009 17:57:50 GMT   (245kb)

Title: Microlensing variability in FBQ 0951+2635: short-timescale events or a
  long-timescale fluctuation?
Authors: V. N. Shalyapin, L. J. Goicoechea, E. Koptelova, B. P. Artamonov, A.
  V. Sergeyev, A. P. Zheleznyak, T. A. Akhunov, O. A. Burkhonov, S. N.
  Nuritdinov, A. Ullan
Categories: astro-ph.GA astro-ph.CO
Comments: 9 pages, 5 figures, 3 tables, accepted for publication in MNRAS
\\
  We present and analyse new R-band frames of the gravitationally lensed double
quasar FBQ 0951+2635. These images were obtained with the 1.5m AZT-22 Telescope
at Maidanak (Uzbekistan) in the 2001-2006 period. Previous results in the R
band (1999-2001 period) and the new data allow us to discuss the dominant kind
of microlensing variability in FBQ 0951+2635. The time evolution of the flux
ratio A/B does not favour the continuous production of short-timescale (months)
flares in the faintest quasar component B (crossing the central region of the
lensing galaxy). Instead of a rapid variability scenario, the observations are
consistent with the existence of a long-timescale fluctuation. The flux ratio
shows a bump in the 2003-2004 period and a quasi-flat trend in more recent
epochs. Apart from the global behaviour of A/B, we study the intra-year
variability over the first semester of 2004, which is reasonably well sampled.
Short-timescale microlensing is not detected in that period. Additional data in
the i band (from new i-band images taken in 2007 with the 2m Liverpool Robotic
Telescope at La Palma, Canary Islands) also indicate the absence of
short-timescale events in 2007.
\\ ( http://arxiv.org/abs/0905.4484 ,  245kb)
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\\
arXiv:0905.4488
Date: Wed, 27 May 2009 18:35:00 GMT   (370kb)

Title: A Three-Point Cosmic Ray Anisotropy Method
Authors: J. D. Hague, B. R. Becker, M. S. Gold, J. A. J. Matthews
Categories: astro-ph.IM
\\
  The two-point angular correlation function is a traditional method used to
search for deviations from expectations of isotropy. In this paper we develop
and explore a statistically descriptive three-point method with the intended
application being the search for deviations from isotropy in the highest energy
cosmic rays. We compare the sensitivity of a two-point method and a
"shape-strength" method for a variety of Monte-Carlo simulated anisotropic
signals. Studies are done with anisotropic source signals diluted by an
isotropic background. Type I and II errors for rejecting the hypothesis of
isotropic cosmic ray arrival directions are evaluated for four different event
sample sizes: 27, 40, 60 and 80 events, consistent with near term data
expectations from the Pierre Auger Observatory. In all cases the ability to
reject the isotropic hypothesis improves with event size and with the fraction
of anisotropic signal. While ~40 event data sets should be sufficient for
reliable identification of anisotropy in cases of rather extreme (highly
anisotropic) data, much larger data sets are suggested for reliable
identification of more subtle anisotropies. The shape-strength method
consistently performs better than the two point method and can be easily
adapted to an arbitrary experimental exposure on the celestial sphere.
\\ ( http://arxiv.org/abs/0905.4488 ,  370kb)
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\\
arXiv:0905.4494
Date: Wed, 27 May 2009 19:38:41 GMT   (10kb)

Title: A Pilot Search for Population III Supernova Candidates in the
  Spitzer/IRAC Dark Field
Authors: Mark I Frost, Jason Surace, Leonidas A Moustakas, Jessica Krick
Categories: astro-ph.CO
Comments: ApJL, in press
\\
  We have undertaken a systematic search for candidate supernovae from
high-redshift Population III stars in a field that has been observed with
repeated imaging on a cadence of 2-3 weeks over a 2.2 year baseline, the
Spitzer/IRAC Dark Field. The individual epochs reach a typical 5-sigma depth of
1 uJy in IRAC Channel 1 (3.6 um). Requiring a minimum of four epochs coverage,
the total effective area searched is 214 sq arcminutes. The unprecedented depth
and multi-epochal nature of these data make it ideal for a first foray to
detect transient objects which may be candidate luminous Pair Instability
Supernovae from the primordial-metallicity first stars. The search was
conducted over a broad range of timescales, allowing for different durations of
the putative candidates' light curve plateau phases. All candidates were vetted
by inspection of the Spitzer imaging data, as well as deep HST/ACS F814W
imaging available over the full field. While many resolved-source objects were
found with Spitzer variability, no transient objects could plausibly be
identified as high-redshift supernovae candidates. The resulting 95% confidence
level upper limit is 23/sq deg/yr, for sources with plateau timescales under
400/(1+z) days and brightnesses above ~1 uJy.
\\ ( http://arxiv.org/abs/0905.4494 ,  10kb)
%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-
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arXiv:0905.3655 (*cross-listing*)
Date: Fri, 22 May 2009 10:32:06 GMT   (8kb)

Title: On the Nature of the Cosmological Constant Problem
Authors: M. D. Maia, A. J. S.Capistrano
Categories: gr-qc astro-ph.CO hep-ex
Comments: LaTex, 5 pages no figutres
Journal-ref: Intl. Jour. Modern Physics A, vol 24, nos 8 & 9 (2009), 1545-1548
\\
  General relativity postulates the Minkowski space-time to be the standard
flat geometry against which we compare all curved space-times and the
gravitational ground state where particles, quantum fields and their vacuum
states are primarily conceived. On the other hand, experimental evidences show
that there exists a non-zero cosmological constant, which implies in a deSitter
space-time, not compatible with the assumed Minkowski structure. Such
inconsistency is shown to be a consequence of the lack of a application
independent curvature standard in Riemann's geometry, leading eventually to the
cosmological constant problem in general relativity.
  We show how the curvature standard in Riemann's geometry can be fixed by
Nash's theorem on locally embedded Riemannian geometries, which imply in the
existence of extra dimensions. The resulting gravitational theory is more
general than general relativity, similar to brane-world gravity, but where the
propagation of the gravitational field along the extra dimensions is a
mathematical necessity, rather than being a a postulate. After a brief
introduction to Nash's theorem, we show that the vacuum energy density must
remain confined to four-dimensional space-times, but the cosmological constant
resulting from the contracted Bianchi identity is a gravitational contribution
which propagates in the extra dimensions. Therefore, the comparison between the
vacuum energy and the cosmological constant in general relativity ceases to be.
Instead, the geometrical fix provided by Nash's theorem suggests that the
vacuum energy density contributes to the perturbations of the gravitational
field.
\\ ( http://arxiv.org/abs/0905.3655 ,  8kb)
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\\
arXiv:0905.4204 (*cross-listing*)
Date: Tue, 26 May 2009 16:46:47 GMT   (6kb)

Title: Is nonrelativistic gravity possible?
Authors: A.A. Kocharyan
Categories: hep-th astro-ph.CO gr-qc math.DS
Comments: 7 pages
\\
  We study nonrelativistic gravity using the Hamiltonian formalism. For the
dynamics of general relativity (relativistic gravity) the formalism is well
known and called the ADM formalism. We show that if the lapse function is
constrained correctly, then nonrelativistic gravity is described by a
consistent Hamiltonian system. Surprisingly, nonrelativistic gravity can have
solutions identical to relativistic gravity ones. In particular, (A)dS black
holes of Einstein gravity and IR limit of Horava gravity are locally identical.
\\ ( http://arxiv.org/abs/0905.4204 ,  6kb)
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\\
arXiv:0905.4239 (*cross-listing*)
Date: Tue, 26 May 2009 17:40:44 GMT   (256kb)

Title: Dark matter direct detection in the MSSM with heavy scalars
Authors: Nicolas Bernal
Categories: hep-ph astro-ph.HE
Comments: 20 pages, 10 figures
Report-no: UB-ECM-PF-09/14, ICCUB-09-205
\\
  We explore the dark matter detection prospects in the Minimal Supersymmetric
Standard Model in the scenario where the scalar partners of the fermions and
the Higgs particles (except for the Standard-Model-like one) are assumed to be
very heavy and are removed from the low-energy spectrum. We analyse the
neutralino LSP ($\chi_1^0$) in scenarios where the gaugino mass parameters are
universal at the GUT scale and also the case where they are non-universal. This
analysis is carried out in the framework of a Xenon-like 100 kg experiment. In
general, an important fraction of the parameter space giving rise to the dark
matter relic density measured by WMAP can be probed and excluded in the case of
not detecting any WIMP. In the opposite case, once a WIMP signal has been
found, we show that for a light $\chi_1^0$ which is a higgsino-gaugino mixture
it is possible to reconstruct efficiently the mass and the scattering
cross-section of the neutralino LSP. Moreover, we show that it is also feasible
to put strong constraints over some of the parameters of the Lagrangian, e.g.
the higgsino and the gaugino mass parameters.
\\ ( http://arxiv.org/abs/0905.4239 ,  256kb)
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arXiv:astro-ph/0507696
replaced with revised version Wed, 27 May 2009 15:27:27 GMT   (117kb)

Title: On the theory of MHD waves in a shear flow of a magnetized turbulent
  plasma
Authors: T. M. Mishonov, Y. G. Maneva, Z. D. Dimitrov and T. S. Hristov
Categories: astro-ph
Comments: 21 pages, 13 figures, PACS: 52.35.Bj, 95.30.Qd, 98.62.Mw, 97.10.Gz,
  47.20.Ft; Analytical solution for the amplification of slow magnetosonic wave
  is given by the confluent Heun function. Minor corrections
\\ ( http://arxiv.org/abs/astro-ph/0507696 ,  117kb)
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\\
arXiv:0807.3334
replaced with revised version Wed, 27 May 2009 16:49:29 GMT   (35kb)

Title: Is a step in the primordial spectral index favored by CMB data ?
Authors: Minu Joy, Arman Shafieloo, Varun Sahni and Alexei A. Starobinsky
Categories: astro-ph gr-qc hep-th
Comments: Several new results, figures and enhanced discussion. Main
  conclusions unchanged. Matches the final version to be published in JCAP
\\ ( http://arxiv.org/abs/0807.3334 ,  35kb)
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\\
arXiv:0809.2016
replaced with revised version Wed, 27 May 2009 11:24:28 GMT   (869kb)

Title: The Imperial IRAS-FSC Redshift Catalogue (IIFSCz)
Authors: Lingyu Wang, Michael Rowan-Robinson
Categories: astro-ph
Comments: 12 pages, 12 figures, 1 table. Revised on 23/04/09. The catalogue has
  been revised to correct the fluxes of extended sources. Accepted for
  publication in MNRAS
\\ ( http://arxiv.org/abs/0809.2016 ,  869kb)
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\\
arXiv:0810.4445
replaced with revised version Wed, 27 May 2009 13:14:56 GMT   (4560kb)

Title: Optical phenomena in brany Kerr spacetimes
Authors: Jan Schee and Zdenek Stuchlik
Categories: astro-ph
Comments: Accepted by Int. Journal of Mod. Phys. D
\\ ( http://arxiv.org/abs/0810.4445 ,  4560kb)
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\\
arXiv:0811.4228
replaced with revised version Wed, 27 May 2009 04:01:38 GMT   (1462kb)

Title: The Adaptive TreePM: An Adaptive Resolution Code for Cosmological N-body
  Simulations
Authors: J. S. Bagla and Nishikanta Khandai (Harish-Chandra Research Institute)
Categories: astro-ph
Comments: 18 pages, 11 figures. Accepted for publication in the MNRAS
\\ ( http://arxiv.org/abs/0811.4228 ,  1462kb)
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\\
arXiv:0812.1025
replaced with revised version Wed, 27 May 2009 19:32:22 GMT   (3380kb,D)

Title: A Map of the Integrated Sachs-Wolfe Signal from Luminous Red Galaxies
Authors: Benjamin R. Granett (IfA Hawaii), Mark C. Neyrinck (JHU, IfA),
  Istv\'an Szapudi (IfA, E\"otv\"os Lor\'and Univ.)
Categories: astro-ph
Comments: 9 pages, 12 figures, accepted to ApJ. Updated discussion about
  redshift cuts
\\ ( http://arxiv.org/abs/0812.1025 ,  3380kb)
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\\
arXiv:0812.4874
replaced with revised version Tue, 26 May 2009 20:00:32 GMT   (891kb,D)

Title: Reaction of Accretion Disks to Abrupt Mass Loss During Binary Black Hole
  Merger
Authors: Sean M. O'Neill, M. Coleman Miller, Tamara Bogdanovic, Christopher S.
  Reynolds, and Jeremy D. Schnittman
Categories: astro-ph
Comments: 14 pages, 5 figures. Accepted for publication in The Astrophysical
  Journal. Minor revisions and improved figures
\\ ( http://arxiv.org/abs/0812.4874 ,  891kb)
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\\
arXiv:0903.0242 (*cross-listing*)
replaced with revised version Wed, 27 May 2009 07:43:03 GMT   (81kb)

Title: High Energy Cosmic Rays from Decaying Supersymmetric Dark Matter
Authors: Koji Ishiwata, Shigeki Matsumoto, Takeo Moroi
Categories: hep-ph astro-ph.HE
Comments: 34 pages, 20 figures, published version
Report-no: TU-840, UT-HET-026
\\ ( http://arxiv.org/abs/0903.0242 ,  81kb)
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\\
arXiv:0903.2386
replaced with revised version Wed, 27 May 2009 15:34:37 GMT   (98kb)

Title: Amplification of Slow Magnetosonic Waves by Shear Flow: Heating and
  Friction Mechanisms of Accretion Disks
Authors: T. M. Mishonov, Z. D. Dimitrov, Y. G. Maneva, and T. S. Hristov
Categories: astro-ph.GA astro-ph.SR
Comments: 26pages, 11 figures, In Space Plasma Physics, Proceedings of the
  School and Workshop on Space Plasma Physics, 31 August--7 September 2008,
  Sozopol, Bulgaria, Editor: I. Zhelyazkov, American Institute of Physics, AIP
  Conference Proceedings (2009). 5 new references are given in version 2.
  Analytical expression for long wavelength amplification
\\ ( http://arxiv.org/abs/0903.2386 ,  98kb)
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\\
arXiv:0905.3039 (*cross-listing*)
replaced with revised version Wed, 27 May 2009 19:14:42 GMT   (51kb)

Title: Hidden Charged Dark Matter
Authors: Jonathan L. Feng, Manoj Kaplinghat, Huitzu Tu, Hai-Bo Yu
Categories: hep-ph astro-ph.CO
Comments: 28 pages; v2: references added
Report-no: UCI-TR-2009-06
\\ ( http://arxiv.org/abs/0905.3039 ,  51kb)
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\\
arXiv:0905.3982
replaced with revised version Wed, 27 May 2009 04:28:46 GMT   (60kb)

Title: Environmental Effects on the Star Formation Activity in Galaxies at
  z=1.2 in the COSMOS Field
Authors: Y. Ideue, T. Nagao, Y. Taniguchi, Y. Shioya, T. Saito, T. Murayama, S.
  S. Sasaki, J. R. Trump, A. M. Koekemoer, H. Aussel, P. Capak, O. Ilbert, H.
  McCracken, B. Mobasher, M. Salvato, D. B. Sanders, and N. Scoville
Categories: astro-ph.CO
Comments: 10pages, 5figures, accepted for publication in ApJ
\\ ( http://arxiv.org/abs/0905.3982 ,  60kb)
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