894 research outputs found
The Impact of Massive Stars on the Formation of Young Stellar Clusters
Massive OB stars play an important role in the evolution of molecular clouds
and star forming regions. The OB stars both photo--ionize molecular gas as well
as sweep up and compress interstellar gas through winds, ionization fronts, and
supernovae. In this contribution, we examine the effect massive stars have on
the formation of young stellar clusters. We first discuss the processes by
which OB stars destroy cluster--forming molecular cores, and hence terminate
star formation. We overview observational evidence that OB stars forming in
young stellar clusters destroy their parental cores on a timescale of 0.1 Myr,
and we discuss some of the implications of this result. We then summarize
extensive observations of the NGC 281 molecular cloud complex, and present
evidence that two types of triggered star formation are occurring in this
complex. Our goal is to underscore the impact massive stars have on cluster
formation over distances ranging from 0.1 pc to 300 pc.Comment: 8 pages, Latex, to appear in "Hot Star Workshop III: The Earliest
Phases of Massive Star Birth" (ed. P.A. Crowther
Hot Gas Structure in the Elliptical Galaxy NGC 4472
We present X-ray spectroscopic and morphological analyses using Chandra ACIS
and ROSAT observations of the giant elliptical galaxy NGC 4472 in the Virgo
cluster. We discuss previously unobserved X-ray structures within the extended
galactic corona. In the inner 2' of the galaxy, we find X-ray holes or cavities
with radii of ~2 kpc, corresponding to the position of radio lobes. These holes
were produced during a period of nuclear activity that began 1.2 x 10^7 years
ago and may be ongoing. We also find an asymmetrical edge in the galaxy X-ray
emission 3' (14 kpc) northeast of the core and an ~8' tail (36 kpc) extending
southwest of the galaxy. These two features probably result from the
interaction of NGC 4472 gas with the Virgo gas, which produces compression in
the direction of NGC 4472's infall and an extended tail from ram pressure
stripping. Assuming the tail is in pressure equilibrium with the surrounding
gas, we compute its angle to our line of sight and estimate that its true
extent exceeds 100 kpc. Finally, in addition to emission from the nucleus
(first detected by Soldatenkov, Vikhlinin & Pavlinsky), we detect two small
extended sources within 10'' of the nucleus of the galaxy, both of which have
luminosities of ~7 x 10^38 erg/s.Comment: 25 pages, 11 figures, accepted by Ap
Direct detection of a substellar companion to the young nearby star PZ Telescopii
Aims: We study the formation of substellar objects (exoplanets and brown
dwarfs) as companions to young nearby stars. Methods: With high contrast AO
imaging obtained with NACO at ESO's VLT we search for faint
companion-candidates around our targets, whose companionship can be confirmed
with astrometry. Results: In the course of our imaging campaign we found a
faint substellar companion of the nearby pre-main sequence star PZ Tel, a
member of the beta Pic moving group. The companion is 5-6 mag fainter than its
host star in JHK and is located at a separation of only 0.3 arcsec (or 15 AU of
projected separation) north-east of PZ Tel. Within three NACO observing epochs
we could confirm common proper motion (>39 sigma) and detected orbital motion
of PZ Tel B around its primary (>37 sigma). The photometry of the newly found
companion is consistent with a brown dwarf with a mass of 24 to 40 MJup, at the
distance (50 pc) and age (8-20 Myr) of PZ Tel. The effective temperature of the
companion, derived from its photometry, ranges between 2500 and 2700 K, which
corresponds to a spectral type between M6 and M8. After beta Pic b, PZ Tel B is
the second closest substellar companion imaged directly around a young star.Comment: accepted for publication in A&A Letter
Characterization of the Benchmark Binary NLTT 33370
We report the confirmation of the binary nature of the nearby, very low-mass
system NLTT 33370 with adaptive optics imaging and present resolved
near-infrared photometry and integrated light optical and near-infrared
spectroscopy to characterize the system. VLT-NaCo and LBTI-LMIRCam images show
significant orbital motion between 2013 February and 2013 April. Optical
spectra reveal weak, gravity sensitive alkali lines and strong lithium 6708
Angstrom absorption that indicate the system is younger than field age.
VLT-SINFONI near-IR spectra also show weak, gravity sensitive features and
spectral morphology that is consistent with other young, very low-mass dwarfs.
We combine the constraints from all age diagnostics to estimate a system age of
~30-200 Myr. The 1.2-4.7 micron spectral energy distribution of the components
point toward T_eff=3200 +/- 500 K and T_eff=3100 +/- 500 K for NLTT 33370 A and
B, respectively. The observed spectra, derived temperatures, and estimated age
combine to constrain the component spectral types to the range M6-M8.
Evolutionary models predict masses of 113 +/- 8 M_Jup and 106 +/- 7 M_Jup from
the estimated luminosities of the components. KPNO-Phoenix spectra allow us to
estimate the systemic radial velocity of the binary. The Galactic kinematics of
NLTT 33370AB are broadly consistent with other young stars in the Solar
neighborhood. However, definitive membership in a young, kinematic group cannot
be assigned at this time and further follow-up observations are necessary to
fully constrain the system's kinematics. The proximity, age, and late-spectral
type of this binary make it very novel and an ideal target for rapid, complete
orbit determination. The system is one of only a few model calibration
benchmarks at young ages and very low-masses.Comment: 25 pages, 3 tables, 13 figures, accepted for publication in The
Astrophysical Journa
How Neutrinos Get Mass and What Other Things May Happen Besides Oscillations
In this talk I address the theoretical issue of what new physics is required
to make . I then discuss what other things may happen besides
neutrino oscillations. In particular I consider a possible new scenario of
leptogenesis in R parity nonconserving supersymmetry.Comment: 7 pages including 1 figure, talk at WHEPP-
A global cloud map of the nearest known brown dwarf
Brown dwarfs -- substellar bodies more massive than planets but not massive
enough to initiate the sustained hydrogen fusion that powers self-luminous
stars -- are born hot and slowly cool as they age. As they cool below about
2,300 K, liquid or crystalline particles composed of calcium aluminates,
silicates and iron condense into atmospheric 'dust', which disappears at still
cooler temperatures (around 1,300 K). Models to explain this dust dispersal
include both an abrupt sinking of the entire cloud deck into the deep, unob-
servable atmosphere and breakup of the cloud into scattered patches (as seen on
Jupiter and Saturn). Thus far, observations of brown dwarfs have been limited
to globally integrated measurements, which can reveal surface inhomogeneities
but cannot unambiguously resolve surface features. Here we report a
two-dimensional map of a brown dwarf's surface that allows identification of
large-scale bright and dark features, indicative of patchy clouds.Comment: 17 pages, 8 figures. Spectra and map available upon reques
Orbital characterization of GJ1108A system, and comparison of dynamical mass with model-derived mass for resolved binaries
We report an orbital characterization of GJ1108Aab that is a low-mass binary
system in pre-main-sequence phase. Via the combination of astrometry using
adaptive optics and radial velocity measurements, an eccentric orbital solution
of =0.63 is obtained, which might be induced by the Kozai-Lidov mechanism
with a widely separated GJ1108B system. Combined with several observed
properties, we confirm the system is indeed young. Columba is the most probable
moving group, to which the GJ1108A system belongs, although its membership to
the group has not been established. If the age of Columba is assumed for
GJ1108A, the dynamical masses of both GJ1108Aa and GJ1108Ab ( and ) are more massive than what an
evolutionary model predicts based on the age and luminosities. We consider the
discrepancy in mass comparison can attribute to an age uncertainty; the system
is likely older than stars in Columba, and effects that are not implemented in
classical models such as accretion history and magnetic activity are not
preferred to explain the mass discrepancy. We also discuss the performance of
the evolutionary model by compiling similar low-mass objects in evolutionary
state based on the literature. Consequently, it is suggested that the current
model on average reproduces the mass of resolved low-mass binaries without any
significant offsets.Comment: Accepted in Ap
Direct Imaging of a Cold Jovian Exoplanet in Orbit around the Sun-like Star GJ 504
Several exoplanets have recently been imaged at wide separations of >10 AU
from their parent stars. These span a limited range of ages (<50 Myr) and
atmospheric properties, with temperatures of 800--1800 K and very red colors (J
- H > 0.5 mag), implying thick cloud covers. Furthermore, substantial model
uncertainties exist at these young ages due to the unknown initial conditions
at formation, which can lead to an order of magnitude of uncertainty in the
modeled planet mass. Here, we report the direct imaging discovery of a Jovian
exoplanet around the Sun-like star GJ 504, detected as part of the SEEDS
survey. The system is older than all other known directly-imaged planets; as a
result, its estimated mass remains in the planetary regime independent of
uncertainties related to choices of initial conditions in the exoplanet
modeling. Using the most common exoplanet cooling model, and given the system
age of 160 [+350, -60] Myr, GJ 504 b has an estimated mass of 4 [+4.5, -1.0]
Jupiter masses, among the lowest of directly imaged planets. Its projected
separation of 43.5 AU exceeds the typical outer boundary of ~30 AU predicted
for the core accretion mechanism. GJ 504 b is also significantly cooler (510
[+30, -20] K) and has a bluer color (J-H = -0.23 mag) than previously imaged
exoplanets, suggesting a largely cloud-free atmosphere accessible to
spectroscopic characterization. Thus, it has the potential of providing novel
insights into the origins of giant planets, as well as their atmospheric
properties.Comment: 20 pages, 12 figures, Accepted for publication in ApJ. Minor updates
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