23,160 research outputs found
Eta Carinae across the 2003.5 Minimum: Analysis in the visible and near infrared spectral region
We present an analysis of the visible through near infrared spectrum of Eta
Carinae and its ejecta obtained during the "Eta Carinae Campaign with the UVES
at the ESO VLT". This is a part of larger effort to present a complete Eta
Carinae spectrum, and extends the previously presented analyses with the
HST/STIS in the UV (1240-3159 A) to 10,430 A. The spectrum in the mid and near
UV is characterized by the ejecta absorption. At longer wavelengths, stellar
wind features from the central source and narrow emission lines from the
Weigelt condensations dominate the spectrum. However, narrow absorption lines
from the circumstellar shells are present. This paper provides a description of
the spectrum between 3060 and 10,430 A, including line identifications of the
ejecta absorption spectrum, the emission spectrum from the Weigelt
condensations and the P-Cygni stellar wind features. The high spectral
resolving power of VLT/UVES enables equivalent width measurements of atomic and
molecular absorption lines for elements with no transitions at the shorter
wavelengths. However, the ground based seeing and contributions of nebular
scattered radiation prevent direct comparison of measured equivalent widths in
the VLT/UVES and HST/STIS spectra. Fortunately, HST/STIS and VLT/UVES have a
small overlap in wavelength coverage which allows us to compare and adjust for
the difference in scattered radiation entering the instruments' apertures. This
paper provides a complete online VLT/UVES spectrum with line identifications
and a spectral comparison between HST/STIS and VLT/UVES between 3060 and 3160
A.Comment: 13 pages, 11 figures + atlas. The paper accepted for the ApJS and is
accompanied with an atlas in the online edition pape
Life Stories and Mental Health: The Role of Identification Processes in Theory and Interventions
The goal of this article is to explore the relations between narratives and mental health from a psychological perspective. We argue that a process of identification with personal experiences underlies narrative structures that are known to be related to mental health. Overidentification and underidentification are described as general processes underlying mental health problems. Gerontological insights in reminiscence and life review and cognitive psychological studies on autobiographical memories validate this claim. Practical applications in mental health care provide even further evidence for the role of identification processes in mental health and how they can be targeted in intervention
ISOGAL-DENIS detection of red giants with weak mass loss in the Galactic Bulge
The ISOGAL project is a survey of the stellar populations, structure, and
recent star formation history of the inner disk and bulge of the Galaxy. ISOGAL
combines 15 and 7micron ISOCAM observations with DENIS IJKs data to determine
the nature of a source and the interstellar extinction. In this paper we report
an ISOGAL study of a small field in the inner Galactic Bulge (l=0deg, b=1.0deg,
area=0.035 sq. deg) as a prototype of the larger area ISOGAL survey of the
inner Galaxy. The five wavelengths of ISOGAL+DENIS, together with the
relatively low and constant extinction in front of this specific field, allow
reliable determination of the nature of the sources. The primary scientific
result of this paper is evidence that the most numerous class of ISOGAL
15micron sources are Red Giants in the Galactic bulge and central disk, with
luminosities just above or close to the RGB tip and weak mass-loss rates. They
form loose sequences in the magnitude-colour diagrams [15]/Ks-[15] and
[15]/[7]-[15]. Their large excesses at 15micron with respect to 2micron and
7micron is due to circumstellar dust produced by mass-loss at low rates. These
ISOGAL results are the first systematic evidence and study of dust emission at
this early stage (''Intermediate'' AGB), before the onset of the large
mass-loss phase. It is thus well established that efficient dust formation is
already associated with such low mass-loss rates during this early phase.Comment: 15 pages, 9 figures, accepted for publication in Astronomy and
Astrophysics Journa
Luminosity Function of the Perigalactocentric Region
We present H and K photometry of 42,000 stars in an area of 250 arcmin
centered on the Galactic center. We use the photometry to construct a
dereddened K band luminosity function (LF) for this region, excluding the
excessively crowded inner 2' of the Galaxy. This LF is intermediate between the
LF of Baade's window and the LF of inner 2' of the Galactic center. We
speculate that the bright stars in this region have an age which is
intermediate between the starburst population in the Galactic center and the
old bulge population. We present the coordinates and mags for 16 stars with
K_{0} < 5 for spectroscopic follow up.Comment: 25 pages. Tarred, gzipped and uuencoded. Includes LaTex source file,
Figures 3 to 9 and 5 Tables. Figures 1 and 2 are available at
ftp://bessel.mps.ohio-state.edu/pub/vijay . Submitted to Ap
CENSORS: A Combined EIS-NVSS Survey Of Radio Sources. I. Sample definition, radio data and optical identifications
A new sample of radio sources, with the designated name CENSORS (A Combined
EIS-NVSS Survey Of Radio Sources), has been defined by combining the NRAO VLA
Sky Survey (NVSS) at 1.4 GHz with the ESO Imaging Survey (EIS) Patch D, a 3 by
2 degree region of sky centred at 09 51 36.0, -21 00 00 (J2000). New radio
observations of 199 NVSS radio sources with NVSS flux densities S(1.4GHz) >
7.8mJy are presented, and compared with the EIS I-band imaging observations
which reach a depth of I~23; optical identifications are obtained for over
two-thirds of the ~150 confirmed radio sources within the EIS field. The radio
sources have a median linear size of 6 arcseconds, consistent with the trend
for lower flux density radio sources to be less extended. Other radio source
properties, such as the lobe flux density ratios, are consistent with those of
brighter radio source samples. From the optical information, 30-40% of the
sources are expected to lie at redshifts z >~ 1.5.
One of the key goals of this survey is to accurately determine the high
redshift evolution of the radio luminosity function. These radio sources are at
the ideal flux density level to achieve this goal; at redshifts z~2 they have
luminosities which are around the break of the luminosity function and so
provide a much more accurate census of the radio source population at those
redshifts than the existing studies of extreme, high radio power sources. Other
survey goals include investigating the dual--population unification schemes for
radio sources, studying the radio luminosity dependence of the evolution of
radio source environments, and understanding the radio power dependence of the
K-z relation for radio galaxies.Comment: Accepted for publication in MNRAS. 28 pages plus 36 reduced
resolution jpeg figures. A postscript version with full resolution figures
included in the text is available from
http://www.roe.ac.uk/~pnb/censors.ps.g
Multiwavelength observations of a giant flare on CN Leonis I. The chromosphere as seen in the optical spectra
Flares on dM stars contain plasmas at very different temperatures and thus
affect a wide wavelength range in the electromagnetic spectrum. While the
coronal properties of flares are studied best in X-rays, the chromosphere of
the star is observed best in the optical and ultraviolet ranges. Therefore,
multiwavelength observations are essential to study flare properties throughout
the atmosphere of a star. We analysed simultaneous observations with UVES/VLT
and XMM-Newton of the active M5.5 dwarf CN Leo (Gl 406) exhibiting a major
flare. The optical data cover the wavelength range from 3000 to 10000 Angstrom.
From our optical data, we find an enormous wealth of chromospheric emission
lines occurring throughout the spectrum. We identify a total of 1143 emission
lines, out of which 154 are located in the red arm, increasing the number of
observed emission lines in this red wavelength range by about a factor of 10.
Here we present an emission line list and a spectral atlas. We also find line
asymmetries for H I, He I, and Ca II lines. For the last, this is the first
observation of asymmetries due to a stellar flare. During the flare onset,
there is additional flux found in the blue wing, while in the decay phase,
additional flux is found in the red wing. We interpret both features as caused
by mass motions. In addition to the lines, the flare manifests itself in the
enhancement of the continuum throughout the whole spectrum, inverting the
normal slope for the net flare spectrum.Comment: 15 pages, accepted by A&
Molecular hydrogen absorption systems in Sloan Digital Sky Survey
We present a systematic search for molecular hydrogen absorption systems at
high redshift in quasar spectra from the Sloan Digital Sky Survey (SDSS) II
Data Release 7 and SDSS-III Data Release 9. We have selected candidates using a
modified profile fitting technique taking into account that the Ly
forest can effectively mimic H absorption systems at the resolution of SDSS
data. To estimate the confidence level of the detections, we use two methods: a
Monte-Carlo sampling and an analysis of control samples. The analysis of
control samples allows us to define regions of the spectral quality parameter
space where H absorption systems can be confidently identified. We find
that H absorption systems with column densities
can be detected in only less than 3% of SDSS quasar spectra. We estimate the
upper limit on the detection rate of saturated H absorption systems () in Damped Ly- (DLA) systems to be about 7%. We
provide a sample of 23 confident H absorption system candidates that would
be interesting to follow up with high resolution spectrographs. There is a
1 color excess and non-significant extinction excess
in quasar spectra with an H candidate compared to standard DLA-bearing
quasar spectra. The equivalent widths (EWs) of C II, Si II and Al III (but not
Fe II) absorptions associated with H candidate DLAs are larger compared to
standard DLAs. This is probably related to a larger spread in velocity of the
absorption lines in the H bearing sample.Comment: 17 pages, 17 figures, accepted for publication in MNRA
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