7,703 research outputs found
Serendipitous discovery of a projected pair of QSOs separated by 4.5 arcsec on the sky
We present the serendipitous discovery of a projected pair of quasi-stellar
objects (QSOs) with an angular separation of arcsec. The
redshifts of the two QSOs are widely different: one, our programme target, is a
QSO with a spectrum consistent with being a narrow line Seyfert 1 AGN at
. For this target we detect Lyman-, \ion{C}{4}, and
\ion{C}{3]}. The other QSO, which by chance was included on the spectroscopic
slit, is a Type 1 QSO at a redshift of , for which we detect
\ion{C}{4}, \ion{C}{3]} and \ion{Mg}{2}. We compare this system to previously
detected projected QSO pairs and find that only about a dozen previously known
pairs have smaller angular separation.Comment: 4 pages, 3 figures. Accepted for publication in A
Orbit Determination of Close Binary Systems using Lucky Imaging
We present relative positions of visual binaries observed during 2009 with
the FastCam "lucky-imaging" camera at the 1.5-m Carlos Sanchez Telescope (TCS)
at the Observatorio del Teide. We obtained 424 CCD observations (averaged in
198 mean relative positions) of 157 binaries with angular separations in the
range 0.14-15.40", with a median separation of 0.51". For a given system, each
CCD image represents the sum of the best 10-25% images from 1000-5000
short-exposure frames. Derived internal errors were 7 mas in r and 1.2^{\circ}
(9 mas) in q. When comparing to systems with very well-known orbits, we find
that the rms deviation in r residuals is 23 mas, while the rms deviation in q
residuals is 0.73 deg/r. We confirmed 18 Hipparcos binaries and we report new
companions to BVD 36 A and J 621 B. For binaries with preliminary orbital
parameters, the relative radial velocity was estimated as well. We also present
four new revised orbits computed for LDS 873, BU 627 A-BC, BU 628 and HO 197
AB. This work is the first results on visual binaries using the FastCam
lucky-imaging camera.Comment: 23 pages, 10 figures, 14 tables, accepted August 18th, 2011, to be
published in MNRA
Ages for illustrative field stars using gyrochronology: viability, limitations and errors
We here develop an improved way of using a rotating star as a clock, set it
using the Sun, and demonstrate that it keeps time well. This technique, called
gyrochronology, permits the derivation of ages for solar- and late-type main
sequence stars using only their rotation periods and colors. The technique is
clarified and developed here, and used to derive ages for illustrative groups
of nearby, late-type field stars with measured rotation periods. We first
demonstrate the reality of the interface sequence, the unifying feature of the
rotational observations of cluster and field stars that makes the technique
possible, and extends it beyond the proposal of Skumanich by specifying the
mass dependence of rotation for these stars. We delineate which stars it cannot
currently be used on. We then calibrate the age dependence using the Sun. The
errors are propagated to understand their dependence on color and period.
Representative age errors associated with the technique are estimated at ~15%
(plus possible systematic errors) for late-F, G, K, & early-M stars. Ages
derived via gyrochronology for the Mt. Wilson stars are shown to be in good
agreement with chromospheric ages for all but the bluest stars, and probably
superior. Gyro ages are then calculated for each of the active main sequence
field stars studied by Strassmeier and collaborators where other ages are not
available. These are shown to be mostly younger than 1Gyr, with a median age of
365Myr. The sample of single, late-type main sequence field stars assembled by
Pizzolato and collaborators is then assessed, and shown to have gyro ages
ranging from under 100Myr to several Gyr, and a median age of 1.2Gyr. Finally,
we demonstrate that the individual components of the three wide binaries
XiBooAB, 61CygAB, & AlphaCenAB yield substantially the same gyro ages.Comment: 58 pages, 18 color figures, accepted for publication in The
Astrophysical Journal; Age uncertainties slightly modified upon correcting an
algebraic error in Section
Spectroscopy at B-factories Using Hard Photon Emission
The process of hard photon emission by initial electrons (positrons) at
B-factories is discussed. It is shown that studies of the bottomonium
spectroscopy will be feasible for the planned integrated luminosity of the
B-factory experiments.Comment: 9 pages, Latex, 1 fugure, Submitted to Int.Jour.Mod.Phys.
Absorption-selected galaxies trace the low-mass, late-type, star-forming population at
We report on the stellar content, half-light radii and star formation rates
of a sample of 10 known high-redshift () galaxies selected on
strong neutral hydrogen (HI) absorption (log(N(HI)/cm) toward
background quasars. We use observations from the {\it Hubble Space Telescope}
(HST) Wide Field Camera 3 in three broad-band filters to study the spectral
energy distribution(SED) of the galaxies. Using careful quasar point spread
function subtraction, we study their galactic environments, and perform the
first systematic morphological characterisation of such absorption-selected
galaxies at high redshifts. Our analysis reveals complex, irregular hosts with
multiple star-forming clumps. At a spatial sampling of 0.067 arcsec per pixel
(corresponding to 0.55 kpc at the median redshift of our sample), 40% of our
sample requires multiple S\'ersic components for an accurate modelling of the
observed light distributions. Placed on the mass-size relation and the `main
sequence' of star-forming galaxies, we find that absorption-selected galaxies
at high redshift extend known relations determined from deep
luminosity-selected surveys to an order of magnitude lower stellar mass, with
objects primarily composed of star-forming, late-type galaxies. We measure
half-light radii in the range 0.4 to 2.6 kpc based on the
reddest band (F160W) to trace the oldest stellar populations, and stellar
masses in the range 8 to 10
derived from fits to the broad-band SED. Spectroscopic and SED-based star
formation rates are broadly consistent, and lie in the range log(SFR/Myr) 0.0 to 1.7.Comment: 17 pages, Accepted for publication in MNRAS. This revision has minor
text change
Astrometric Methods and Instrumentation to Identify and Characterize Extrasolar Planets: A Review
I present a review of astrometric techniques and instrumentation utilized to
search for, detect, and characterize extra-solar planets. First, I briefly
summarize the properties of the present-day sample of extrasolar planets, in
connection with predictions from theoretical models of planet formation and
evolution. Next, the generic approach to planet detection with astrometry is
described, with significant discussion of a variety of technical, statistical,
and astrophysical issues to be faced by future ground-based as well as
space-borne efforts in order to achieve the required degree of measurement
precision. After a brief summary of past and present efforts to detect planets
via milli-arcsecond astrometry, I then discuss the planet-finding capabilities
of future astrometric observatories aiming at micro-arcsecond precision.
Lastly, I outline a number experiments that can be conducted by means of
high-precision astrometry during the next decade, to illustrate its potential
for important contributions to planetary science, in comparison with other
indirect and direct methods for the detection and characterization of planetary
systems.Comment: 61 pages, 8 figures, PASP, accepted (October 2005 issue
Constraints on a Massive Dirac Neutrino Model
We examine constraints on a simple neutrino model in which there are three
massless and three massive Dirac neutrinos and in which the left handed
neutrinos are linear combinations of doublet and singlet neutrinos. We examine
constraints from direct decays into heavy neutrinos, indirect effects on
electroweak parameters, and flavor changing processes. We combine these
constraints to examine the allowed mass range for the heavy neutrinos of each
of the three generations.Comment: latex, 29 pages, 7 figures (not included), MIT-CTP-221
The Zeta Herculis binary system revisited. Calibration and seismology
We have revisited the calibration of the visual binary system Zeta Herculis
with the goal to give the seismological properties of the G0 IV sub-giant Zeta
Her A. We have used the most recent physical and observational data. For the
age we have obtained 3387 Myr, for the masses respectively 1.45 and 0.98 solar
mass, for the initial helium mass fraction 0.243, for the initial mass ratio of
heavy elements to hydrogen 0.0269 and for the mixing-length parameters
respectively 0.92 and 0.90 using the Canuto & Mazitelli (1991, 1992) convection
theory. Our results do not exclude that Zeta Her A is itself a binary
sub-system; the mass of the hypothetical unseen companion would be smaller than
0.05 solar mass. The adiabatic oscillation spectrum of Zeta Her A is found to
be a complicated superposition of acoustic and gravity modes; some of them have
a dual character. This greatly complicates the classification of the non-radial
modes. The echelle diagram used by the observers to extract the frequencies
will work for ell=0, 2, 3. The large difference is found to be of the order of
42 mu Hz, in agreement with the Martic et al. (2001) seismic observations.Comment: 12 pages, A&A in pres
A T8.5 Brown Dwarf Member of the Xi Ursae Majoris System
The Wide-field Infrared Survey Explorer has revealed a T8.5 brown dwarf (WISE
J111838.70+312537.9) that exhibits common proper motion with a
solar-neighborhood (8 pc) quadruple star system - Xi Ursae Majoris. The angular
separation is 8.5 arc-min, and the projected physical separation is about 4000
AU. The sub-solar metallicity and low chromospheric activity of Xi UMa A argue
that the system has an age of at least 2 Gyr. The infrared luminosity and color
of the brown dwarf suggests the mass of this companion ranges between 14 and 38
Jupiter masses for system ages of 2 and 8 Gyr respectively.Comment: AJ in press, 12 pages LaTeX with 6 figures. More astrometric data and
a laser guide star adaptive optics image adde
Stellar Multiplicity and the IMF: Most Stars Are Single
In this short communication I compare recent findings suggesting a low binary
star fraction for late type stars with knowledge concerning the forms of the
stellar initial and present day mass functions for masses down to the hydrogen
burning limit. This comparison indicates that most stellar systems formed in
the galaxy are likely single and not binary as has been often asserted. Indeed,
in the current epoch two-thirds of all main sequence stellar systems in the
Galactic disk are composed of single stars. Some implications of this
realization for understanding the star and planet formation process are briefly
mentioned.Comment: Accepted for publication in the Astrophysical Journal Letters, 5
pages, 2 figures. Complete paper can be also obtained at
http://www.cfa.harvard.edu/~clada/pubs_html/binaries.htm
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