First, Second and Third Massive Stars in Open Clusters

The goal of this paper is to study possibilities of using first, second and third massive stars in open clusters to estimate total cluster mass and membership. We built estimator functions with the use of numerical simulations and analytical approximations and studied the precision and error distribution of the obtained estimator functions. We found that the distribution of the mass of first, second and third massive stars shows strong power-law tails at the high-mass end, thus it is better to use median or mode values instead of average ones. We show that the third massive star is a much better estimator then the first as it is more precise and less dependent on parameters such as maximum allowed stellar mass.Comment: 24 pages, 5 figures, 5 tables, to appear in Ap

Higgs boson search significance deformations due to mixed-in scalars

The existence of exotic scalars that mix with the Standard Model (SM) Higgs boson can affect Higgs boson phenomenology in a multitude of ways. We consider two light Higgs bosons with shared couplings to SM fields and with masses close to each other, in the range where the h \to WW \to l \nu l \nu is an important search channel. In this channel, we do not find the dilution of significance of the `SM-like' Higgs boson that is naively expected because of the mixing. This is because of leakage of events from the decay of the other scalar into its signal region. Nevertheless, we show that the broadening of the h\to WW \to l \nu l \nu significance plots of Standard Model Higgs boson searches could indicate the first evidence of the the extra scalar state.Comment: 6 pages, 6 figures; v2: all plots now made with the lighter Higgs mass equal to 125 GeV and other minor corrections made, to be published in Physics Letters

A Unified tool to estimate Distances, Ages and Masses (UniDAM) from spectrophotometric data

Galactic archaeology - the study of the formation and evolution of the Milky Way by reconstructing its past from its current constituents - requires precise and accurate knowledge of stellar parameters for as many stars as possible. To achieve this a number of large spectroscopic surveys have been undertaken and are still ongoing. So far consortia carrying out the different spectroscopic surveys have used different tools to determine stellar parameters of stars from their derived effective temperatures (Teff), surface gravities (log g) and metallicities ([Fe/H]) possibly combined with photometric, astrometric, interferometric or asteroseismic information. Here we aim to homogenise the stellar characterisation by applying a unified tool to a large set of publicly available spectrophotometric data. We use spectroscopic data from a variety of large surveys combined with infra-red photometry from 2MASS and AllWISE and compare these in a Bayesian manner with PARSEC isochrones to derive probability density functions (PDFs) for stellar masses, ages and distances. We treat PDFs of pre-helium-core burning, helium-core burning and post helium-core burning solutions as well as different peaks in multi-modal PDFs (i.e. each unimodal sub-PDF) of the different evolutionary phases separately. For over 2.5 million stars we report mass, age and distance estimate for each evolutionary phase and unimodal sub-PDF. We report Gaussian, skewed Gaussian, truncated Gaussian, modified truncated exponential distribution or truncated Student's t-distribution functions to represent each sub-PDF, allowing to reconstruct detailed PDFs. Comparisons with stellar parameter estimates from the literature show good agreement within uncertainties. We present UniDAM - the unified tool applicable to spectrophotometric data of different surveys to obtain a homogenised set of stellar parameters

A close look at the Centaurus A group of galaxies: I. Metallicity distribution functions and population gradients in early-type dwarfs

We study dwarf galaxies in the Centaurus A group to investigate their metallicity and possible environmental effects. The Centaurus A group (at ~4 Mpc from the Milky Way) contains about 50 known dwarf companions of different morphologies and stellar contents, thus making it a very interesting target to study how these galaxies evolve. Here we present results for the early-type dwarf galaxy population in this group. We use archival HST/ACS data to study the resolved stellar content of 6 galaxies, together with isochrones from the Dartmouth stellar evolutionary models. We derive photometric metallicity distribution functions of stars on the upper red giant branch via isochrone interpolation. The 6 galaxies are moderately metal-poor (=-1.56 to -1.08), and metallicity spreads are observed (internal dispersions of sigma_[Fe/H]=0.10 to 0.41 dex). We also investigate the possible presence of intermediate-age stars, and discuss how these affect our results. The dwarfs exhibit flat to weak radial metallicity gradients. For the two most luminous, most metal-rich galaxies, we find statistically significant evidence for at least two stellar subpopulations: the more metal-rich stars are found in the center of the galaxies, while the metal-poor ones are more broadly distributed within the galaxies. We find no clear trend of the derived physical properties as a function of (present-day) galaxy position in the group, which may be due to the small sample we investigate. We compare our results to the early-type dwarf population of the Local Group, and find no outstanding differences, despite the fact that the Centaurus A group is a denser environment that is possibly in a more advanced dynamical stage.Comment: 21 pages, 12 figures, accepted for publication in Astronomy and Astrophysic