753 research outputs found
The discovery of a low mass, pre-main-sequence stellar association around gamma Velorum
We report the serendipitous discovery of a population of low mass, pre-main
sequence stars (PMS) in the direction of the Wolf-Rayet/O-star binary system
gamma^{2} Vel and the Vela OB2 association. We argue that gamma^{2} Vel and the
low mass stars are truly associated, are approximately coeval and that both are
at distances between 360-490 pc, disagreeing at the 2 sigma level with the
recent Hipparcos parallax of gamma^{2} Vel, but consistent with older distance
estimates. Our results clearly have implications for the physical parameters of
the gamma^{2} Vel system, but also offer an exciting opportunity to investigate
the influence of high mass stars on the mass function and circumstellar disc
lifetimes of their lower mass PMS siblings.Comment: Monthly Notices of the Royal Astronomical Society, Letters - in pres
Membership, metallicity and lithium abundances for solar-type stars in NGC 6633
We present spectroscopic observations of candidate F, G and K type stars in
NGC 6633, an open cluster with a similar age to the Hyades. We identify 10 new
cluster members including one short period binary system. Combining this survey
with that of Jeffries (1997), we identify a total of 30 solar-type members. We
have used the F and early G stars to spectroscopically estimate
[Fe/H]=-0.096+/-0.081 for NGC 6633 and with more precision that NGC 6633 has
(0.074+/-0.041) dex less iron than the Pleiades and (0.206+/-0.040) dex less
iron than the Hyades. Lithium abundances have been estimated for the NGC 6633
members and compared with consistently determined Li abundances in other
clusters. Several mid F stars in NGC 6633 show strong Li depletion at
approximately the same effective temperature that this phenomenon is seen in
the Hyades. At cooler temperatures the Li abundance patterns in several open
clusters with similar ages (NGC 6633, Hyades, Praesepe and Coma Berenices) are
remarkably similar, despite their differing [Fe/H]. There is however evidence
that the late G and K stars of NGC 6633 have depleted less Li than their Hyades
counterparts. This qualitatively agrees with models for pre-main sequence Li
depletion that feature only convective mixing, but these models cannot
simultaneously explain why these stars have in turn depleted Li by more than 1
dex compared with their ZAMS counterparts in the Pleiades. Two explanations are
put forward. The first is that elemental abundance ratios, particularly [O/Fe],
may have non-solar values in NGC 6633 and would have to be higher than in
either the Hyades or Pleiades. The second is that additional non-convective
mixing, driven by angular momentum loss, causes additional photospheric Li
depletion during the first few hundred Myr of main sequence evolution.Comment: Accepted for MNRAS - some figures are compressed, a better version
can be found at http://www.astro.keele.ac.uk/~rdj
The CH fraction of Carbon stars at high Galactic latitudes
CH stars form a distinct class of objects with characteristic properties like
iron deficiency, enrichment of carbon and overabundance in heavy elements.
These properties can provide strong observational constraints for theoretical
computation of nucleosynthesis at low-metallicity. An important question is the
relative surface density of CH stars which can provide valuable inputs to our
understanding on the role of low to intermediate-mass stars in the early
Galactic chemical evolution. Spectroscopic characterization provides an
effective way of identifying CH stars. The present analysis is aimed at a
quantitative assessment of the fraction of CH stars in a sample of stars using
a set of spectral classification criteria. The sample consists of 92 objects
selected from a collection of candidate Faint High Latitude Carbon stars from
the Hamburg/ESO survey. Medium resolution (R ~ 1300) spectra for these objects
were obtained using OMR at VBO, Kavalur and HFOSC at HCT, IAO, Hanle, during
2007 - 2009 spanning a wavelength range 3800 - 6800 A. Spectral analysis shows
36 of the 92 objects to be potential CH stars; combined with our earlier
studies (Goswami 2005, Goswami et al. 2007) this implies ~ 37% (of 243) objects
as the CH fraction. We present spectral descriptions of the newly identified CH
star candidates. Estimated effective temperatures, 12C/13C isotopic ratios and
their locations on the two colour J-H vs H-K plot are used to support their
identification.Comment: 18 pages, 8 figures,Accepted for publication in MNRA
Recommended from our members
Large-strain quasi-static compression materials tests in support of penetration modeling research
Target penetration by projectiles typically generates large strains, at least locally. Hence, accurate analytic modeling of penetration demands that constitutive models be calibrated using large strain material test data. Tensile test data is limited by specimen necking (the Considere criterion), restricting attainable strains. Linear extrapolation of tensile data to target strains can seriously overestimate the material flow stress, resulting in erroneously stiff analytical predictions. That is, other tests which can attain larger strains often reveal a continually decreasing tangent modulus at large strains. We report quasistatic room temperature compression tests approaching true strains of {var epsilon} = {minus}1. A few tensile tests are included to illustrate the previous point. Materials tested are 7075-T651, 5083-H131, and 6061-T651 aluminum alloys, 4340 steel and X21-C tungsten alloy. 7 refs., 6 figs
APM 08279+5255: an ultraluminous BAL quasar at a redshift z=3.87
We report on the discovery of a highly luminous, broad absorption line quasar
at a redshift of which is positionally coincident, within one
arcsecond, with the IRAS FSC source F08279+5255. A chance alignment of the
quasar and the IRAS source is extremely unlikely and we argue that the optical
and FIR flux are different manifestations of the same object. With an R-band
magnitude of 15.2, and an IRAS 60\mum flux of 0.51\jy, APM 08279+5255 is
(apparently) easily the most intrinsically luminous object known, with
L_{Bol}\sim5\times10^{15}L_{\odot}}. Imaging suggests that gravitational
lensing may play a role in amplifying the intrinsic properties of the system.
The optical spectrum of the quasar clearly reveals the presence of three
potential lensing galaxies, \mg absorption systems at and ,
and a \ly absorption system at . We estimate the total amplification of
the optical component to be , but, due to the larger scale of the
emitting region, would expect the infrared amplification to be significantly
less. Even making the conservative assumption that all wavelengths are
amplified by a factor 40, APM 08279+5255 still possesses a phenomenal
luminosity of \simgt 10^{14L_{\odot}}, indicating that it belongs to a small,
but significant population of high--redshift, hyperluminous objects with
copious infrared emission.Comment: 15 Pages with Four figures. Accepted for publication in the
Astrophysical Journa
Submillimeter Observations of the Ultraluminous BAL Quasar APM 08279+5255
With an inferred bolometric luminosity of 5\times10^{15}{\rm \lsun}, the
recently identified z=3.87, broad absorption line quasar APM 08279+5255 is
apparently the most luminous object currently known. As half of its prodigious
emission occurs in the infrared, APM 08279+5255 also represents the most
extreme example of an Ultraluminous Infrared Galaxy. Here, we present new
submillimeter observations of this phenomenal object; while indicating that a
vast quantity of dust is present, these data prove to be incompatible with
current models of emission mechanisms and reprocessing in ultraluminous
systems. The influence of gravitational lensing upon these models is considered
and we find that while the emission from the central continuum emitting region
may be significantly enhanced, lensing induced magnification cannot easily
reconcile the models with observations. We conclude that further modeling,
including the effects of any differential magnification is required to explain
the observed emission from APM 08279+5255.Comment: 12 Pages with Two figures. Accepted for publication in the
Astrophysical Journal Letter
A Process and Outcome Evaluation of a Shelter for Homeless Young Women
To evaluate the processes and outcomes of a short-term shelter, both quantitative and qualitative data were gathered via participant observation, focus group interviews with shelter staff and residents, and individual interviews with a sample of 40 young women who had been homeless prior to using the shelter. The process evaluation showed that the shelter staff strived to utilize an empowerment philosophy in their relationships with residents, but that there were many challenges to implementing this philosophy. The outcome evaluation showed that, at a 3-month follow-up, the participants reported significant improvements in housing, income, independence, and life satisfaction, but most continued to experience poverty and a number of other difficulties. The results were discussed in terms of the implications for future research and the value and limitations of shelters for dealing with homeless youth. The need for more sustained and comprehensive program interventions and supportive social policies was underscored
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