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Technical Review of Residential Programmable Communicating Thermostat Implementation for Title 24-2008
Providing stringent star formation rate limits of z2 QSO host galaxies at high angular resolution
We present integral field spectrograph (IFS) with laser guide star adaptive
optics (LGS-AO) observations of z=2 quasi-stellar objects (QSOs) designed to
resolve extended nebular line emission from the host galaxy. Our data was
obtained with W. M. Keck and Gemini-North Observatories using OSIRIS and NIFS
coupled with the LGS-AO systems. We have conducted a pilot survey of five QSOs,
three observed with NIFS+AO and two observed with OSIRIS+AO at an average
redshift of z=2.15. We demonstrate that the combination of AO and IFS provides
the necessary spatial and spectral resolutions required to separate QSO
emission from its host. We present our technique for generating a PSF from the
broad-line region of the QSO and performing PSF subtraction of the QSO emission
to detect the host galaxy. We detect H and [NII] for two sources, SDSS
J1029+6510 and SDSS J0925+06 that have both star formation and extended
narrow-line emission. Assuming that the majority of narrow-line H is
from star formation, we infer a star formation rate for SDSS J1029+6510 of 78.4
Myr originating from a compact region that is kinematically
offset by 290 - 350 km/s. For SDSS J0925+06 we infer a star formation rate of
29 Myr distributed over three clumps that are spatially offset
by 7 kpc. The null detections on three of the QSOs are used to infer
surface brightness limits and we find that at 1.4 kpc distance from the QSO
that the un-reddened star formation limit is 0.3
Myrkpc. If we assume a typical extinction values for z=2
type-1 QSOs, the dereddened star formation rate for our null detections would
be 0.6 Myrkpc. These IFS observations indicate that
if star formation is present in the host it would have to occur diffusely with
significant extinction and not in compact, clumpy regions.Comment: 17 pages, 7 figures, 7 tables, Accepted to Ap
on’t Take My Breath Away: A Case of High-Risk Pulmonary Embolism in the Setting of Patent Foramen Ovale Requiring Extracorporeal Membrane Oxygenation
Prospects for measuring supermassive black hole masses with future extremely large telescopes
The next generation of giant-segmented mirror telescopes ( 20 m) will
enable us to observe galactic nuclei at much higher angular resolution and
sensitivity than ever before. These capabilities will introduce a revolutionary
shift in our understanding of the origin and evolution of supermassive black
holes by enabling more precise black hole mass measurements in a mass range
that is unreachable today. We present simulations and predictions of the
observations of nuclei that will be made with the Thirty Meter Telescope (TMT)
and the adaptive optics assisted integral-field spectrograph IRIS, which is
capable of diffraction-limited spectroscopy from band (0.9 m) to
band (2.2 m). These simulations, for the first time, use realistic values
for the sky, telescope, adaptive optics system, and instrument, to determine
the expected signal-to-noise ratio of a range of possible targets spanning
intermediate mass black holes of \msun to the most massive black
holes known today of . We find that IRIS will be able to
observe Milky Way-mass black holes out the distance of the Virgo cluster, and
will allow us to observe many more brightest cluster galaxies where the most
massive black holes are thought to reside. We also evaluate how well the
kinematic moments of the velocity distributions can be constrained at the
different spectral resolutions and plate scales designed for IRIS. We find that
a spectral resolution of will be necessary to measure the masses of
intermediate mass black holes. By simulating the observations of galaxies found
in SDSS DR7, we find that over massive black holes will be observable at
distances between with the estimated sensitivity and angular
resolution provided by access to -band (0.9 m) spectroscopy from IRIS
and the TMT adaptive optics system. (Abridged)Comment: 19 pages, 20 figures, accepted to A
Clinical Depression Pathway Implementation: Outcomes From Pilot Practices
In 2017, an estimated 17.3 million adults (7.1%) in the United States had at least one major depressive episode. Although there are known, effective treatments for depression, fewer than half of those affected receive such treatments. LVHN implemented an Ambulatory Clinical Depression Pathway at three pilot sites to improve depression screening, symptom management, remission documentation, and patient quality of life. The pathway utilized the PHQ-9 metric for evaluating and tracking severity of depression while providing guidelines for short- and long-term follow up, patient education, and medical management. Five hundred twenty-five individuals were screened during the 6-month pilot study; 38% were diagnosed with depression (PHQ Score =5). Of those, 82% were prescribed antidepressant medications and 60% received education. Over-the-phone follow up for moderately-severe to severe patients occurred in 28% of encounters, while in-office follow up was completed within 6 months for 32% of depressed patients. Seventy three percent of patients who followed up showed improvement in depression with a 15% rate of complete remission. One site’s decreased adherence (58% screened, 24% in-office follow up) resulted in less response in more severe depression
Retired A Stars: The Effect of Stellar Evolution on the Mass Estimates of Subgiants
Doppler surveys have shown that the occurrence rate of Jupiter-mass planets
appears to increase as a function of stellar mass. However, this result depends
on the ability to accurately measure the masses of evolved stars. Recently,
Lloyd (2011) called into question the masses of subgiant stars targeted by
Doppler surveys. Lloyd argues that very few observable subgiants have masses
greater than 1.5 Msun, and that most of them have masses in the range 1.0-1.2
Msun. To investigate this claim, we use Galactic stellar population models to
generate an all-sky distribution of stars. We incorporate the effects that make
massive subgiants less numerous, such as the initial mass function and
differences in stellar evolution timescales. We find that these effects lead to
negligibly small systematic errors in stellar mass estimates, in contrast to
the roughly 50% errors predicted by Lloyd. Additionally, our simulated target
sample does in fact include a significant fraction of stars with masses greater
than 1.5 Msun, primarily because the inclusion of an apparent magnitude limit
results in a Malmquist-like bias toward more massive stars, in contrast to the
volume-limited simulations of Lloyd. The magnitude limit shifts the mean of our
simulated distribution toward higher masses and results in a relatively smaller
number of evolved stars with masses in the range 1.0-1.2 Msun. We conclude
that, within the context of our present-day understanding of stellar structure
and evolution, many of the subgiants observed in Doppler surveys are indeed as
massive as main-sequence A stars.Comment: Accepted to ApJ, 5 pages, 3 figures; changed title, reworded
introduction and conclusion
Retired A Stars and Their Companions: Exoplanets Orbiting Three Intermediate-Mass Subgiants
We report precision Doppler measurements of three intermediate-mass subgiants
from Lick and Keck Observatories. All three stars show variability in their
radial velocities consistent with planet-mass companions in Keplerian orbits.
We find a planet with a minimum mass of 2.5 Mjup in a 351.5 day orbit around HD
192699, a planet with a minimum mass of 2.0 Mjup in a 341.1 day orbit around HD
210702, and a planet with a minimum mass of 0.61 Mjup in a 297.3 day orbit
around HD 175541. Stellar mass estimates from evolutionary models indicate that
all of these stars were formerly A-type dwarfs with masses ranging from 1.65 to
1.85 Msun. These three long-period planets would not have been detectable
during their stars' main-sequence phases due to the large rotational velocities
and stellar jitter exhibited by early-type dwarfs. There are now 9 "retired"
(evolved) A-type stars (Mstar > 1.6 Msun) with known planets. All 9 planets
orbit at distances a \geq 0.78 AU, which is significantly different than the
semimajor axis distribution of planets around lower-mass stars. We examine the
possibility that the observed lack of close-in planets is due to engulfment by
their expanding host stars, but we find that this explanation is inadequate
given the relatively small stellar radii of K giants (Rstar < 32 Rsun = 0.15
AU) and subgiants (Rstar < 7 Rsun = 0.03 AU). Instead, we conclude that planets
around intermediate-mass stars reside preferentially beyond ~0.8 AU, which may
be a reflection of different formation and migration histories of planets
around A-type stars.Comment: 31 pages, 9 figures, 6 tables, ApJ accepted, corrected minor typo
Behavior problems and prevalence of asthma symptoms among Brazilian children.
OBJECTIVE: Asthma is the most common chronic disease in childhood and has been designated a public health problem due to the increase in its prevalence in recent decades, the amount of health service expenditure it absorbs and an absence of consensus about its etiology. The relationships among psychosocial factors and the occurrence, symptomatology, and severity of asthma have recently been considered. There is still controversy about the association between asthma and a child's mental health, since the pathways through which this relationship is established are complex and not well researched. This study aims to investigate whether behavior problems are associated with the prevalence of asthma symptoms in a large urban center in Latin America. METHODS: It is a cross-section study of 869 children between 6 and 12 years old, residents of Salvador, Brazil. The International Study of Allergy and Asthma in Childhood (ISAAC) instrument was used to evaluate prevalence of asthma symptoms. The Child Behavior Checklist (CBCL) was employed to evaluate behavioral problems. RESULTS: 19.26% (n=212) of the children presented symptoms of asthma. 35% were classified as having clinical behavioral problems. Poisson's robust regression model demonstrated a statistically significant association between the presence of behavioral problems and asthma symptoms occurrence (PR: 1.43; 95% CI: 1.10-1.85). CONCLUSION: These results suggest an association between behavioral problems and pediatric asthma, and support the inclusion of mental health care in the provision of services for asthma morbidity
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