1,218 research outputs found
Limits on the infrared photometric monitoring of brown dwarfs
Recent monitoring programs of ultra cool field M and L dwarfs (low mass stars
or brown dwarfs) have uncovered low amplitude photometric I-band variations
which may be associated with an inhomogeneous distribution of photospheric
condensates. Further evidence hints that this distribution may evolve on very
short timescales, specifically of order a rotation period or less. In an
attempt to study this behaviour in more detail, we have carried out a pilot
program to monitor three L dwarfs in the near infrared where these objects are
significantly brighter than at shorter wavelengths. We present a robust data
analysis method for improving the precision and reliability of infrared
photometry. No significant variability was detected in either the J or Km bands
in 2M1439 and SDSS1203 above a peak-to-peak amplitude of 0.04 mag (0.08 mag for
2M1112). The main limiting factor in achieving lower detection limits is
suspected to be second order extinction effects in the Earth's atmosphere, on
account of the very different colours of the target and reference stars.
Suggestions are given for overcoming such effects which should improve the
sensitivity and reliability of infrared variability searches.Comment: MNRAS, in press (9 pages
The Real Estate Investment Trust: State Law Problems
We present a map of the three-dimensional (3D) distribution of dust in the Orion complex. Orion is the closest site of high-mass star formation, making it an excellent laboratory for studying the interstellar medium and star formation. We used data from the Gaia-TGAS catalogue combined with photometry from 2MASS and WISE to get the distances and extinctions of individual stars in the vicinity of the Orion complex. We use a Gaussian process and adopt a non-parametric method to infer the probability distribution function of the dust densities at arbitrary points throughout the region. We map the dust distribution towards different parts of the Orion complex. We find that the distance and depth of the cloud are compatible with other recent works, which show that the method can be applicable to local molecular clouds to map their 3D dust distribution. We also demonstrate the danger of only using colours of stars to derive their extinctions without considering further physical constraints, such as the colour-magnitude diagram (CMD)
The Mass Dependence of Stellar Rotation in the Orion Nebula Cluster
We have determined new rotation periods for 404 stars in the Orion Nebula
Cluster using the Wide Field Imager attached to the MPG/ESO 2.2 m telescope on
La Silla, Chile. Mass estimates are available for 335 of these and most have M
< 0.3 M_sun. We confirm the existence of a bimodal period distribution for the
higher mass stars in our sample and show that the median rotation rate
decreases with increasing mass for stars in the range 0.1 < M <0.4 M_sun. While
the spread in angular momentum (J) at any given mass is more than a factor of
10, the majority of lower mass stars in the ONC rotate at rates approaching 30%
of their critical break-up velocity, as opposed to 5-10% for solar-like stars.
This is a consequence of both a small increase in observed specific angular
momentum (j=J/M) and a larger decrease in the critical value of j with
decreasing mass. Perhaps the most striking fact, however, is that j varies by
so little - less than a factor of two - over the interval 0.1-1.0 M_sun. The
distribution of rotation rates with mass in the ONC (age ~ 1 My) is similar in
nature to what is found in the Pleiades (age ~ 100 My). These observations
provide a significant new guide and test for models of stellar angular momentum
evolution during the proto-stellar and pre-main sequence phases.Comment: 11 pages, 3 figure
New stellar encounters discovered in the second Gaia data release
Passing stars may play an important role in the evolution of our solar
system. We search for close stellar encounters to the Sun among all 7.2 million
stars in Gaia-DR2 that have six-dimensional phase space data. We characterize
encounters by integrating their orbits through a Galactic potential and
propagating the correlated uncertainties via a Monte Carlo resampling. After
filtering to remove spurious data, we find 694 stars that have median (over
uncertainties) closest encounter distances within 5 pc, all occurring within 15
Myr from now. 26 of these have at least a 50% chance of coming closer than 1 pc
(and 7 within 0.5 pc), all but one of which are newly discovered here. We
further confirm some and refute several other previously-identified encounters,
confirming suspicions about their data. The closest encounter in the sample is
Gl 710, which has a 95% probability of coming closer than 0.08 pc (17 000 AU).
Taking mass estimates from Gaia astrometry and multiband photometry for
essentially all encounters, we find that Gl 710 also has the largest impulse on
the Oort cloud. Using a Galaxy model, we compute the completeness of the
Gaia-DR2 encountering sample as a function of perihelion time and distance.
Only 15% of encounters within 5 pc occurring within +/- 5 Myr of now have been
identified, mostly due to the lack of radial velocities for faint and/or cool
stars. Accounting for the incompleteness, we infer the present rate of
encounters within 1 pc to be 19.7 +/- 2.2 per Myr, a quantity expected to scale
quadratically with the encounter distance out to at least several pc.
Spuriously large parallaxes in our sample from imperfect filtering would tend
to inflate both the number of encounters found and this inferred rate. The
magnitude of this effect is hard to quantify.Comment: 12 pages. Accepted to A&A. Added to this version: section 3.2 and
Fig. 8 (CMD) with discussion of astrometric quality metrics; full versions of
tables 2 and 3 as ancillary dat
Inferring the three-dimensional distribution of dust in the Galaxy with a non-parametric method: Preparing for Gaia
We present a non-parametric model for inferring the three-dimensional (3D)
distribution of dust density in the Milky Way. Our approach uses the extinction
measured towards stars at different locations in the Galaxy at approximately
known distances. Each extinction measurement is proportional to the integrated
dust density along its line-of-sight. Making simple assumptions about the
spatial correlation of the dust density, we can infer the most probable 3D
distribution of dust across the entire observed region, including along sight
lines which were not observed. This is possible because our model employs a
Gaussian Process to connect all lines-of-sight. We demonstrate the capability
of our model to capture detailed dust density variations using mock data as
well as simulated data from the Gaia Universe Model Snapshot. We then apply our
method to a sample of giant stars observed by APOGEE and Kepler to construct a
3D dust map over a small region of the Galaxy. Due to our smoothness constraint
and its isotropy, we provide one of the first maps which does not show the
"fingers of god" effect.Comment: Minor changes applied. Final version accepted for publication in A&A.
15 pages, 17 figure
Natural Coronagraphic Observations of the Eclipsing T Tauri System KH 15D: Evidence for Accretion and Bipolar Outflow in a WTTS
We present high resolution (R 44,000) UVES spectra of the eclipsing
pre-main sequence star KH 15D covering the wavelength range 4780 to 6810 {\AA}
obtained at three phases: out of eclipse, near minimum light and during egress.
The system evidently acts like a natural coronagraph, enhancing the contrast
relative to the continuum of hydrogen and forbidden emission lines during
eclipse. At maximum light the H equivalent width was 2 {\AA} and
the profile showed broad wings and a deep central absorption. During egress the
equivalent width was much higher (70 {\AA}) and the broad wings, which
extend to 300 km/s, were prominent. During eclipse totality the
equivalent width was less than during egress (40 {\AA}) and the high
velocity wings were much weaker. H showed a somewhat different behavior,
revealing only the blue-shifted portion of the high velocity component during
eclipse and egress. [OI] 6300, 6363 lines are easily seen both
out of eclipse and when the photosphere is obscured and exhibit little or no
flux variation with eclipse phase. Our interpretation is that KH 15D, although
clearly a weak-line T Tauri star by the usual criteria, is still accreting
matter from a circumstellar disk, and has a well-collimated bipolar jet. As the
knife-edge of the occulting matter passes across the close stellar environment
it is evidently revealing structure in the magnetosphere of this pre-main
sequence star with unprecedented spatial resolution. We also show that there is
only a small, perhaps marginally significant, change in the velocity of the K7
star between the maximum light and egress phases probed here
VAMP: semantic validation for MPEG-7 profile descriptions
MPEG-7 can be used to create complex and comprehensive metadata descriptions of multimedia content. Since MPEG-7 is defined in terms of an XML schema, the semantics of its elements has no formal grounding. In addition, certain features can be described in multiple ways. MPEG-7 profiles are subsets of the standard that apply to specific application areas and that aim to reduce this syntactic variability, but they still lack formal semantics. We propose an approach for expressing the semantics explicitly
Plausible home stars of the interstellar object 'Oumuamua found in Gaia DR2
The first detected interstellar object 'Oumuamua that passed within 0.25au of
the Sun on 2017 September 9 was presumably ejected from a stellar system. We
use its newly determined non-Keplerian trajectory together with the
reconstructed Galactic orbits of 7 million stars from Gaia DR2 to identify past
close encounters. Such an "encounter" could reveal the home system from which
'Oumuamua was ejected. The closest encounter, at 0.60pc (0.53-0.67pc, 90%
confidence interval), was with the M2.5 dwarf HIP 3757 at a relative velocity
of 24.7km/s, 1Myr ago. A more distant encounter (1.6pc) but with a lower
encounter (ejection) velocity of 10.7km/s was with the G5 dwarf HD 292249,
3.8Myr ago. Two more stars have encounter distances and velocities intermediate
to these. The encounter parameters are similar across six different
non-gravitational trajectories for 'Oumuamua. Ejection of 'Oumuamua by
scattering from a giant planet in one of the systems is plausible, but requires
a rather unlikely configuration to achieve the high velocities found. A binary
star system is more likely to produce the observed velocities. None of the four
home candidates have published exoplanets or are known to be binaries. Given
that the 7 million stars in Gaia DR2 with 6D phase space information is just a
small fraction of all stars for which we can eventually reconstruct orbits, it
is a priori unlikely that our current search would find 'Oumuamua's home star
system. As 'Oumuamua is expected to pass within 1pc of about 20 stars and brown
dwarfs every Myr, the plausibility of a home system depends also on an
appropriate (low) encounter velocity.Comment: Accepted to The Astronomical Journa
Subcellular Trafficking and Functional Relationship of the HSV-1 Glycoproteins N and M
The herpes simplex virus type 1 (HSV-1) glycoprotein N (gN/UL49.5) is a type I transmembrane protein conserved throughout the herpesvirus family. gN is a resident of the endoplasmic reticulum that in the presence of gM is translocated to the trans Golgi network. gM and gN are covalently linked by a single disulphide bond formed between cysteine 46 of gN and cysteine 59 of gM. Exit of gN from the endoplasmic reticulum requires the N-terminal core of gM composed of eight transmembrane domains but is independent of the C-terminal extension of gM. Co-transport of gN and gM to the trans Golgi network also occurs upon replacement of conserved cysteines in gM and gN, suggesting that their physical interaction is mediated by covalent and non-covalent forces. Deletion of gN/UL49.5 using bacterial artificial chromosome (BAC) mutagenesis generated mutant viruses with wild-type growth behaviour, while full deletion of gM/UL10 resulted in an attenuated phenotype. Deletion of gN/UL49.5 in conjunction with various gM/UL10 mutants reduced average plaque sizes to the same extent as either single gM/UL10 mutant, indicating that gN is nonessential for the function performed by gM. We propose that gN functions in gM-dependent as well as gM-independent processes during which it is complemented by other viral factors
Subcellular Trafficking and Functional Relationship of the HSV-1 Glycoproteins N and M
The herpes simplex virus type 1 (HSV-1) glycoprotein N (gN/UL49.5) is a type I transmembrane protein conserved throughout the herpesvirus family. gN is a resident of the endoplasmic reticulum that in the presence of gM is translocated to the trans Golgi network. gM and gN are covalently linked by a single disulphide bond formed between cysteine 46 of gN and cysteine 59 of gM. Exit of gN from the endoplasmic reticulum requires the N-terminal core of gM composed of eight transmembrane domains but is independent of the C-terminal extension of gM. Co-transport of gN and gM to the trans Golgi network also occurs upon replacement of conserved cysteines in gM and gN, suggesting that their physical interaction is mediated by covalent and non-covalent forces. Deletion of gN/UL49.5 using bacterial artificial chromosome (BAC) mutagenesis generated mutant viruses with wild-type growth behaviour, while full deletion of gM/UL10 resulted in an attenuated phenotype. Deletion of gN/UL49.5 in conjunction with various gM/UL10 mutants reduced average plaque sizes to the same extent as either single gM/UL10 mutant, indicating that gN is nonessential for the function performed by gM. We propose that gN functions in gM-dependent as well as gM-independent processes during which it is complemented by other viral factors
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