2,120 research outputs found
Three Additional Quiescent Low-Mass X-ray Binary Candidates in 47 Tucanae
We identify through their X-ray spectra one certain (W37) and two probable
(W17 and X4) quiescent low-mass X-ray binaries (qLMXBs) containing neutron
stars in a long Chandra X-ray exposure of the globular cluster 47 Tucanae, in
addition to the two previously known qLMXBs. W37's spectrum is dominated by a
blackbody-like component consistent with radiation from the hydrogen atmosphere
of a 10 km neutron star. W37's lightcurve shows strong X-ray variability which
we attribute to variations in its absorbing column depth, and eclipses with a
probable 3.087 hour period. For most of our exposures, W37's blackbody-like
emission (assumed to be from the neutron star surface) is almost completely
obscured, yet some soft X-rays (of uncertain origin) remain. Two additional
candidates, W17 and X4, present X-ray spectra dominated by a harder component,
fit by a power-law of photon index ~1.6-3. An additional soft component is
required for both W17 and X4, which can be fit with a 10 km hydrogen-atmosphere
neutron star model. X4 shows significant variability, which may arise from
either its power-law or hydrogen-atmosphere spectral component. Both W17 and X4
show rather low X-ray luminosities, Lx(0.5-10 keV)~5*10^{31} ergs/s. All three
candidate qLMXBs would be difficult to identify in other globular clusters,
suggesting an additional reservoir of fainter qLMXBs in globular clusters that
may be of similar numbers as the group of previously identified objects. The
number of millisecond pulsars inferred to exist in 47 Tuc is less than 10 times
larger than the number of qLMXBs in 47 Tuc, indicating that for typical
inferred lifetimes of 10 and 1 Gyr respectively, their birthrates are
comparable.Comment: Accepted for publication in ApJ. 13 pages, 7 figures (2 color
Kinematic structure in the young Sigma Orionis association
We have used precise radial velocity measurements for a large number of
candidate low-mass stars and brown dwarfs, to show that the young Sigma Ori
``cluster'' consists of two spatially superimposed components which are
kinematically separated by 7 km/s in radial velocity, and which have different
mean ages. We examine the relationship of these two kinematic groups to other
populations in the Orion OB1 association and briefly discuss the consequence of
mixed age samples for ongoing investigations of the formation and evolution of
low-mass objects in this much-observed region.Comment: MNRAS Letter in pres
Membership, binarity and accretion among very low-mass stars and brown dwarfs of the Sigma Orionis cluster
Intermediate resolution (R=7000) spectroscopy is presented for 76
photometrically selected very low mass (0.04<M<0.3M_{sun}) candidate members of
the Sigma Orionis cluster. More than two thirds appear to be genuine cluster
members on the basis of Li I absorption, weak Na I features and radial
velocities. Photometric selection alone therefore appears to be very effective
in identifying cluster members in this mass range. Only 6 objects appear to be
certain non-members, however a substantial subset of 13 have ambiguous or
contradictory indications of membership and lack Li absorption. Four candidate
binary cluster members are identified. Consideration of sampling and precision
leads us to conclude that either the fraction of very low mass stars and brown
dwarfs in small separation (a<1au) binary systems is larger than in field
M-dwarfs, or the distribution of separations is much less skewed towards large
separations. This conclusion hinges critically on the correct identification of
the small number of binary candidates, but is significant even when only
Li-rich candidate members are considered. Broadened H alpha emission,
indicative of circum(sub)stellar accretion discs is found in 5 or 6 of the
candidate cluster members, 3 of which probably have substellar masses. The
fraction of accretors (10+/-5 per cent) is similar to that found in stars of
higher mass in the cluster using H alpha emission as a diagnostic, but much
lower than found for very low mass stars and brown dwarfs of younger clusters.
The timescale for accretion rates to drop to less than 10^{-11} M_sun/yr is
hence less than the age of the Sigma Ori cluster (3 to 7 Myr) for most low-mass
objects (abridged).Comment: Accepted for publication in MNRA
Another Faint UV Object Associated with a Globular Cluster X-Ray Source: The Case of M92
The core of the metal poor Galactic Globular Cluster M92 (NGC 6341) has been
observed with WFPC2 on the Hubble Space Telescope through visual, blue and
mid-UV filters in a program devoted to study the evolved stellar population in
a selected sample of Galactic Globular Clusters. In the UV color magnitude diagram we have discovered a faint `UV-dominant'
object. This star lies within the error box of a Low Luminosity Globular
Cluster X-ray source (LLGCX) recently found in the core of M92. The properties
of the UV star discovered in M92 are very similar to those of other UV stars
found in the core of some clusters (M13, 47 Tuc, M80, etc)---all of them are
brighter in the UV than in the visible and are located in the vicinity of a
LLGCX. We suggest that these stars are a new sub-class of cataclysmic
variables.Comment: 21 pages, 4 figures. Astrophysical journal in pres
Design and integration of the HARPS3 software system
We present the design of the HARPS3 software system-A distributed, event-driven control system for robotic operation of the HARPS3 spectrograph at the Isaac Newton Telescope (INT). We also describe our approach to integrating the control software components incrementally at various stages of development, using a simulation framework. HARPS3 will be a high resolution (R = 115, 000) echelle spectrograph operating at wavelengths from 380 nm to 690 nm, with a design based on the successful HARPS and HARPS-N instruments. It is being built as part of the Terra Hunting Experiment (THE)-A planned 10 year radial velocity measurement programme to discover Earth-like exoplanets around Sun-like stars
The stellar association around Gamma Velorum and its relationship with Vela OB2
We present the results of a photometric BVI survey of 0.9 square degrees
around the Wolf-Rayet binary gamma^2 Vel and its early-type companion gamma^1
Vel. Several hundred PMS stars are identified and the youth of a subset of
these is confirmed by the presence of lithium, H-alpha emission and X-ray
activity. We show that the PMS stars are kinematically coherent and spatially
concentrated around gamma Vel. The PMS stars have similar proper motions to
gamma Vel, to main-sequence stars around gammaVel and to early-type stars of
the wider Vela OB2 association of which gamma^2 Vel is the brightest member.
The ratio of main-sequence stars to low-mass (0.1-0.6 Msun) PMS stars is
consistent with a Kroupa mass function. Main-sequence fitting to stars around
gamma Vel gives a distance modulus of 7.76+/-0.07 mag, consistent with a
similarly-determined distance for Vela OB2 and with interferometric distances
to gamma^2 Vel. High-mass stellar models indicate an age of 3-4 Myr for gamma^2
Vel, but the low-mass PMS stars have ages of ~10 Myr according to low-mass
evolutionary models and 5-10 Myr by empirically placing them in an age sequence
with other clusters based on colour-magnitude diagrams and lithium depletion.
We conclude that the low-mass PMS stars form a genuine association with gamma
Vel and that this is a subcluster within the larger Vela OB2 association. We
speculate that gamma^2 Vel formed after the low-mass stars, expelling gas,
terminating star formation and unbinding the association. The velocity
dispersion of the PMS stars is too low for this star forming event to have
produced all the stars in Vela OB2. Instead, star formation must have started
at several sites within a molecular cloud, either sequentially or,
simultaneously after some triggering event [abridged].Comment: Accepted for publication in MNRA
Diagrams for heat kernel expansions
A diagramatic heat kernel expansion technique is presented. The method is
especially well suited to the small-derivative expansion of the heat kernel,
but it can also be used to reproduce the results obtained by the approach known
as covariant perturbation theory. The new technique gives an expansion for the
heat kernel at coincident points. It can also be used to obtain the derivative
of the heat kernel and this is useful for evaluating the expectation values of
the stress-energy tensor.Comment: 17 pages, 4 figures, ReVTe
The Herschel Comprehensive (U)LIRG Emission Survey (HerCULES): CO Ladders, fine structure lines, and neutral gas cooling
(Ultra) Luminous Infrared Galaxies ((U)LIRGs) are objects characterized by
their extreme infrared (8-1000 m) luminosities (L and L). The Herschel Comprehensive ULIRG
Emission Survey (HerCULES; PI van der Werf) presents a representative
flux-limited sample of 29 (U)LIRGs that spans the full luminosity range of
these objects (10). With the \emph{Herschel
Space Observatory}, we observe [CII] 157 m, [OI] 63 m, and [OI] 145
m line emission with PACS, CO J=4-3 through J=13-12, [CI] 370 m, and
[CI] 609 m with SPIRE, and low-J CO transitions with ground-based
telescopes. The CO ladders of the sample are separated into three classes based
on their excitation level. In 13 of the galaxies, the [OI] 63 m emission
line is self absorbed. Comparing the CO excitation to the IRAS 60/100 m
ratio and to far infrared luminosity, we find that the CO excitation is more
correlated to the far infrared colors. We present cooling budgets for the
galaxies and find fine-structure line flux deficits in the [CII], [SiII], [OI],
and [CI] lines in the objects with the highest far IR fluxes, but do not
observe this for CO . In order to study the heating of the
molecular gas, we present a combination of three diagnostic quantities to help
determine the dominant heating source. Using the CO excitation, the CO J=1-0
linewidth, and the AGN contribution, we conclude that galaxies with large CO
linewidths always have high-excitation CO ladders, and often low AGN
contributions, suggesting that mechanical heating is important
Signatures of warm carbon monoxide in protoplanetary discs observed with Herschel SPIRE
Molecular gas constitutes the dominant mass component of protoplanetary discs. To date, these sources have not been studied comprehensively at the longest far-infrared and shortest submillimetre wavelengths. This paper presents Herschel SPIRE FTS spectroscopic observations towards 18 protoplanetary discs, covering the entire 450-1540 GHz (666-195 μm) range at ν/Δν ≈ 400-1300. The spectra reveal clear detections of the dust continuum and, in six targets, a significant amount of spectral line emission primarily attributable to 12CO rotational lines. Other targets exhibit little to no detectable spectral lines. Low signal-to-noise detections also include signatures from 13CO, [C i] and HCN. For completeness, we present upper limits of non-detected lines in all targets, including low-energy transitions of H2O and CH+ molecules. The 10 12CO lines that fall within the SPIRE FTS bands trace energy levels of∼50-500 K. Combined with lower and higher energy lines from the literature, we compare the CO rotational line energy distribution with detailed physical-chemical models, for sources where these are available and published. Our 13CO line detections in the disc around Herbig Be star HD 100546 exceed, by factors of∼10-30, the values predicted by a model that matches a wealth of other observational constraints, including the SPIRE 12CO ladder. To explain the observed 12CO/13CO ratio, it may be necessary to consider the combined effects of optical depth and isotope selective (photo)chemical processes. Considering the full sample of 18 objects, we find that the strongest line emission is observed in discs around Herbig Ae/Be stars, although not all show line emission. In addition, two of the six T Tauri objects exhibit detectable 12CO lines in the SPIRE rang
Signatures of warm carbon monoxide in protoplanetary discs observed with Herschel SPIRE
Molecular gas constitutes the dominant mass component of protoplanetary discs. To date, these sources have not been studied comprehensively at the longest far-infrared and shortest submillimetre wavelengths. This paper presents Herschel SPIRE FTS spectroscopic observations towards 18 protoplanetary discs, covering the entire 450-1540 GHz (666-195 μm) range at ν/Δν ≈ 400-1300. The spectra reveal clear detections of the dust continuum and, in six targets, a significant amount of spectral line emission primarily attributable to 12CO rotational lines. Other targets exhibit little to no detectable spectral lines. Low signal-to-noise detections also include signatures from 13CO, [C I] and HCN. For completeness, we present upper limits of non-detected lines in all targets, including low-energy transitions of H2O and CH+ molecules. The 10 12CO lines that fall within the SPIRE FTS bands trace energy levels of ˜50-500 K. Combined with lower and higher energy lines from the literature, we compare the CO rotational line energy distribution with detailed physical-chemical models, for sources where these are available and published. Our 13CO line detections in the disc around Herbig Be star HD 100546 exceed, by factors of ˜10-30, the values predicted by a model that matches a wealth of other observational constraints, including the SPIRE 12CO ladder. To explain the observed 12CO/13CO ratio, it may be necessary to consider the combined effects of optical depth and isotope selective (photo)chemical processes. Considering the full sample of 18 objects, we find that the strongest line emission is observed in discs around Herbig Ae/Be stars, although not all show line emission. In addition, two of the six T Tauri objects exhibit detectable 12CO lines in the SPIRE range
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