Decade of Decline: A Survey of Employer Health Insurance Coverage in New York State

Presents findings from a survey of New York-based firms on trends in employer-sponsored coverage during the recession, including offer rates, eligibility, take-up, and coverage rates; premiums; employer and employee costs; and support for reform measures

Retiree Health Benefits After Medicare Part D: A Snapshot of Prescription Drug Coverage

Based on employer surveys, assesses how the introduction of the Medicare Part D prescription drug benefit affected employer-based retiree, drug, and other health coverage

The Commonwealth Fund/National Opinion Research Center Survey of Retiree Health Benefits, 2005: A Chartbook

Analyzes the state of retiree health benefits, based on a survey of public and private employers. Looks at the Medicare Part D Prescription Drug Benefit, Governmental Accounting Standards Board regulations, and past and future changes to retiree benefits

Small Employer Perspectives On The Affordable Care Act's Premiums, SHOP Exchanges, And Self-Insurance

Beginning January 1, 2014, small businesses having no more than fifty full-time-equivalent workers will be able to obtain healthinsurance for their employees through Small Business Health OptionsProgram (SHOP) exchanges in every state. Although the Affordable Care Act intended the exchanges to make the purchasing of insurance moreattractive and affordable to small businesses, it is not yet known how they will respond to the exchanges. Based on a telephone survey of 604 randomly selected private firms having 3 -- 50 employees, we found that both firms that offered health coverage and those that did not rated most features of SHOP exchanges highly but were also very price sensitive.More than 92 percent of nonoffering small firms said that if they were to offer coverage, it would be "very" or "somewhat" important to them that premium costs be less than they are today. Eighty percent of offering firms use brokers who commonly perform functions of benefit managers -- functions that the SHOP exchanges may assume. Twenty-six percent of firms using brokers reported discussing self-insuring with their brokers. An increase in the number of self-insured small employers could pose a threat to SHOP exchanges and other small-group insurance reforms

Consumer Cost-Sharing in Marketplace vs. Employer Health Insurance Plans, 2015

Using data from 49 states and Washington, D.C., we analyzed changes in costsharing under health plans offered to individuals and families through state and federal exchanges from 2014 to 2015. We examined eight vehicles for cost-sharing, including deductibles, copayments, coinsurance, and out-of-pocket limits, and compared findings with cost-sharing under employer-based insurance. We found cost-sharing under marketplace plans remained essentially unchanged from 2014 to 2015. Stable premiums during that period do not reflect greater costs borne by enrollees. Further, 56 percent of enrollees in marketplace plans attained cost-sharing reductions in 2015. However, for people without cost-sharing reductions, average copayments, deductibles, and out-of-pocket limits under catastrophic, bronze, and silver plans are considerably higher than under employerbased plans on average, while cost-sharing under gold plans is similar employer-based plans on average. Marketplace plans are far more likely than employer-based plans to require enrollees to meet deductibles before they receive coverage for prescription drugs

Using H-alpha Morphology and Surface Brightness Fluctuations to Age-Date Star Clusters in M83

We use new WFC3 observations of the nearby grand design spiral galaxy M83 to develop two independent methods for estimating the ages of young star clusters. The first method uses the physical extent and morphology of Halpha emission to estimate the ages of clusters younger than tau ~10 Myr. It is based on the simple premise that the gas in very young (tau < few Myr) clusters is largely coincident with the cluster stars, is in a small, ring-like structure surrounding the stars in slightly older clusters (e.g., tau ~5 Myr), and is in a larger ring-like bubble for still older clusters (i.e., ~5-10 Myr). The second method is based on an observed relation between pixel-to-pixel flux variations within clusters and their ages. This method relies on the fact that the brightest individual stars in a cluster are most prominent at ages around 10 Myr, and fall below the detection limit (i.e., M_V < -3.5) for ages older than about 100 Myr. These two methods are the basis for a new morphological classification system which can be used to estimate the ages of star clusters based on their appearance. We compare previous age estimates of clusters in M83 determined from fitting UBVI Halpha measurements using predictions from stellar evolutionary models with our new morphological categories and find good agreement at the ~95% level. The scatter within categories is ~0.1 dex in log tau for young clusters (10 Myr) clusters. A by-product of this study is the identification of 22 "single-star" HII regions in M83, with central stars having ages ~4 Myr.Comment: 33 pages, 10 figures, 3 tables; published in March Ap

The Luminosity, Mass, and Age Distributions of Compact Star Clusters in M83 Based on HST/WFC3 Observations

The newly installed Wide Field Camera 3 (WFC3) on the Hubble Space Telescope has been used to obtain multi-band images of the nearby spiral galaxy M83. These new observations are the deepest and highest resolution images ever taken of a grand-design spiral, particularly in the near ultraviolet, and allow us to better differentiate compact star clusters from individual stars and to measure the luminosities of even faint clusters in the U band. We find that the luminosity function for clusters outside of the very crowded starburst nucleus can be approximated by a power law, dN/dL \propto L^{alpha}, with alpha = -2.04 +/- 0.08, down to M_V ~ -5.5. We test the sensitivity of the luminosity function to different selection techniques, filters, binning, and aperture correction determinations, and find that none of these contribute significantly to uncertainties in alpha. We estimate ages and masses for the clusters by comparing their measured UBVI,Halpha colors with predictions from single stellar population models. The age distribution of the clusters can be approximated by a power-law, dN/dt propto t^{gamma}, with gamma=-0.9 +/- 0.2, for M > few x 10^3 Msun and t < 4x10^8 yr. This indicates that clusters are disrupted quickly, with ~80-90% disrupted each decade in age over this time. The mass function of clusters over the same M-t range is a power law, dN/dM propto M^{beta}, with beta=-1.94 +/- 0.16, and does not have bends or show curvature at either high or low masses. Therefore, we do not find evidence for a physical upper mass limit, M_C, or for the earlier disruption of lower mass clusters when compared with higher mass clusters, i.e. mass-dependent disruption. We briefly discuss these implications for the formation and disruption of the clusters.Comment: 36 pages, 13 figures, 1 table; accepted for publication in the Astrophysical Journa

Employer Health Benefits 2008 Annual Survey

Presents annual survey data on the health plans employers offer, including plan types, providers, premiums, coverage, eligibility, enrollment patterns, employee cost-sharing, prescription drug benefits, retiree benefits, and employer opinions

Star formation in 30 Doradus

Using observations obtained with the Wide Field Camera 3 (WFC3) on board the Hubble Space Telescope (HST), we have studied the properties of the stellar populations in the central regions of 30 Dor, in the Large Magellanic Cloud. The observations clearly reveal the presence of considerable differential extinction across the field. We characterise and quantify this effect using young massive main sequence stars to derive a statistical reddening correction for most objects in the field. We then search for pre-main sequence (PMS) stars by looking for objects with a strong (> 4 sigma) Halpha excess emission and find about 1150 of them over the entire field. Comparison of their location in the Hertzsprung-Russell diagram with theoretical PMS evolutionary tracks for the appropriate metallicity reveals that about one third of these objects are younger than ~4Myr, compatible with the age of the massive stars in the central ionising cluster R136, whereas the rest have ages up to ~30Myr, with a median age of ~12Myr. This indicates that star formation has proceeded over an extended period of time, although we cannot discriminate between an extended episode and a series of short and frequent bursts that are not resolved in time. While the younger PMS population preferentially occupies the central regions of the cluster, older PMS objects are more uniformly distributed across the field and are remarkably few at the very centre of the cluster. We attribute this latter effect to photoevaporation of the older circumstellar discs caused by the massive ionising members of R136.Comment: 15 pages, 12 figures. Accepted for publication in The Astrophysical Journa