70 research outputs found
Trumpler 20 - an old and rich open cluster
We show that the open cluster Trumpler 20, contrary to the earlier findings, is actually an old Galactic open cluster. New CCD photometry and high-resolution spectroscopy are used to derive the main parameters of this cluster. At [Fe/H]=â0.11 for a single red giant star, the metallicity is slightly subsolar. The best fit to the colour-magnitude diagrams is achieved using a 1.3-Gyr isochrone with convective overshoot. The cluster appears to have a significant reddening at E(BâV) = 0.46 (for B0 spectral type), although for red giants this high reddening yields the colour temperature exceeding the spectroscopic Teff by about 200 K. Trumpler 20 is a very rich open cluster, containing at least 700 members brighter than MV=+4. It may extend over the field of view available in our study at 20 Ă 20 arcmin
SPACE TELESCOPE SCIENCE
We present the results and measurement of Charge Transfer Efficiency (CTE) of the WFC3 UVIS detector, based on data acquired during the monthly internal Extended Pixel Edge Response (EPER) observations over a 2 year period. We present an algorithm for CTE assessment and fit a power-law to CTE measures versus signal level. We find that at each signal level, CTE declines linearly over time and CTE losses are worst at the lowest signal levels. 1
New Photometric Calibration of the Wide Field Camera 3 Detectors
We present a new photometric calibration of the WFC3-UVIS and WFC3-IR
detectors based on observations collected from 2009 to 2020 for four white
dwarfs, namely GRW+70~5824, GD~153, GD~71, G191B2B, and a G-type star, P330E.
These calibrations include recent updates to the Hubble Space Telescope primary
standard white dwarf models and a new reference flux for Vega. Time-dependent
inverse sensitivities for the two WFC3-UVIS chips, UVIS1 and UVIS2, were
calculated for all 42 full-frame filters, after accounting for temporal changes
in the observed count rates with respect to a reference epoch in 2009. We also
derived new encircled energy values for a few filters and improved sensitivity
ratios for the two WFC3-UVIS chips by correcting for sensitivity changes with
time. Updated inverse sensitivity values for the 20 WFC3-UVIS quad filters and
for the 15 WF3-IR filters were derived by using the new models for the primary
standards and the new Vega reference flux and, in the case of the IR detector,
new flat fields. However, these values do not account for any sensitivity
changes with time. The new calibration provides a photometric internal
precision better than 0.5% for the wide-, medium-, and narrow-band WFC3-UVIS
filters, 5% for the quad filters, and 1% for the WFC3-IR filters. As of October
15, 2020, an updated set of photometric keywords are populated in the WFC3
image headers.Comment: 38 pages, 23 figures, accepted for publication on the Astronomical
Journa
Trumpler 20 - an old and rich open cluster
We show that the open cluster Trumpler 20, contrary to the earlier findings,
is actually an old Galactic open cluster. New CCD photometry and
high-resolution spectroscopy are used to derive the main parameters of this
cluster. At [Fe/H]=-0.11 for a single red giant star, the metallicity is
slightly subsolar. The best fit to the color-magnitude diagrams is achieved
using a 1.3 Gyr isochrone with convective overshoot. The cluster appears to
have a significant reddening at E(B-V)=0.46 (for B0 spectral type), although
for red giants this high reddening yields the color temperature exceeding the
spectroscopic T_eff by about 200 K. Trumpler 20 is a very rich open cluster,
containing at least 700 members brighter than M_V=+4. It may extend over the
field-of-view available in our study at 20'x20'.Comment: 7 pages, 5 figures; accepted for publication in MNRA
Chromosome maps of young LMC clusters: An additional case of coeval multiple populations
Recent studies have revealed that the Multiple Populations (MPs) phenomenon
does not occur only in ancient and massive Galactic globular clusters (GCs),
but it is also observed in external galaxies, where GCs sample a wide age range
with respect to the Milky Way. However, for a long time, it was unclear whether
we were looking at the same phenomenon in different environments or not. The
first evidence that the MPs phenomenon is the same regardless of cluster age
and host galaxy came out recently when an intermediate-age cluster from the
Small Magellanic Cloud, Lindsay 1, and a Galactic GC have been directly
compared. By complementing those data with new images from the Hubble Space
Telescope (HST), we extend the comparison to two clusters of different ages:
NGC 2121 (2.5Gyr) and NGC 1783 (1.5Gyr), from the Large Magellanic
Cloud. We find a clear correlation between the RGB width in the pseudo-colour
and the age of the cluster itself, with the older
cluster having larger and vice-versa.
Unfortunately, the values cannot be directly linked to the N-abundance
variations within the clusters before properly taking account the effect of the
first dredge-up. Such HST data also allow us to explore whether multiple
star-formation episodes occurred within NGC 2121. The two populations are
indistinguishable, with an age difference of only 612 Myr and an initial
Helium spread of 0.02 or lower. This confirms our previous results, putting
serious constraints on any model proposed to explain the origin of the chemical
anomalies in GCs.Comment: 12 pages, 7 figures, 1 table. Accepted for publication in MNRA
Chromosome maps of young LMC clusters: An additional case of coeval multiple populations
Recent studies have revealed that the Multiple Populations (MPs) phenomenon does not occur only in ancient and massive Galactic globular clusters (GCs), but it is also observed in external galaxies, where GCs sample a wide age range with respect to the Milky Way. However, for a long time, it was unclear whether we were looking at the same phenomenon in different environments or not. The first evidence that the MPs phenomenon is the same regardless of cluster age and host galaxy came out recently when an intermediate-age cluster from the Small Magellanic Cloud, Lindsay 1, and a Galactic GC have been directly compared. By complementing those data with new images from the Hubble Space Telescope (HST), we extend the comparison to two clusters of different ages: NGC 2121 (2.5Gyr) and NGC 1783 (1.5Gyr), from the Large Magellanic Cloud. We find a clear correlation between the RGB width in the pseudo-colour and the age of the cluster itself, with the older cluster having larger and vice-versa. Unfortunately, the values cannot be directly linked to the N-abundance variations within the clusters before properly taking account the effect of the first dredge-up. Such HST data also allow us to explore whether multiple star-formation episodes occurred within NGC 2121. The two populations are indistinguishable, with an age difference of only 612 Myr and an initial Helium spread of 0.02 or lower. This confirms our previous results, putting serious constraints on any model proposed to explain the origin of the chemical anomalies in GCs
The Distance to the Hyades Cluster Based on Hubble Space Telescope Fine Guidance Sensor Parallaxes
Trigonometric parallax observations made with the Hubble Space Telescope (HST) Fine Guidance Sensor (FGS) 3 of seven Hyades members in six ïŹelds of view have been analyzed along with their proper motions to determine the distance to the cluster. Knowledge of the convergent point and mean proper motion of the Hyades is critical to the derivation of the distance to the center of the cluster. Depending on the choice of the proper-motion system, the derived cluster center distance varies by 9%. Adopting a reference distance of 46.1 pc or m ÏȘ M Ï 3.32, which is derived from the ground-based parallaxes in the General Catalogue of Trigonometric Stellar Parallaxes (1995 edition), the FK5/PPM proper-motion system yields a distance 4% larger, while the Hanson system yields a distance 2% smaller. The HST FGS parallaxes reported here yield either a 14% or 5% larger distance, depending on the choice of the proper-motion system. Orbital parallaxes (Torres et al.) yield an average distance 4% larger than the reference distance. The variation in the distance derived from the HST data illustrates the importance of the proper-motion system and the individual proper motions to the derivation of the distance to the Hyades center; therefore, a full utilization of the HST FGS parallaxes awaits the establishment of an accurate and consistent proper-motion system
Discovery of astrometric accelerations by dark companions in the globular cluster Ï Centauri
We present results from the search for astrometric accelerations of stars in Ï Centauri using 13 years of regularly-scheduled Hubble Space Telescope WFC3/UVIS calibration observations in the cluster core. The high-precision astrometry ofâŒ160000 sources was searched for significant deviations from linear proper motion. This led to the discovery of four cluster members and one foreground field star with compelling acceleration patterns. We interpret them as the result of the gravitational pull by an invisible companion and determined preliminary Keplerian orbit parameters, including the companionâs mass. For the cluster members our analysis suggests periods ranging from 8.8 to 19+ years and dark companions in the mass range of âŒ0.7toâŒ1.4Mâ. At least one companion could exceed the upper mass-boundary of white dwarfs and can be classified as a neutron-star candidate
Leveraging HST with MUSE: II. Na-abundance variations in intermediate age star clusters
Ancient (10 Gyr) globular clusters (GCs) show chemical abundance variations in the form of patterns among certain elements, e.g. N correlates with Na and anti-correlates with O. Recently, N abundance spreads have also been observed in massive star clusters that are significantly younger than old GCs, down to an age of 2 Gyr. However, so far N has been the only element found to vary in such young objects. We report here the presence of Na abundance variations in the intermediate age massive star clusters NGC 416 (6.5 Gyr old) and Lindsay 1 (7.5 Gyr old) in the Small Magellanic Cloud, by combining HST and ESO-VLT MUSE observations. Using HST photometry we were able to construct ''chromosome maps'' and separate sub-populations with different N content, in the red giant branch of each cluster. MUSE spectra of individual stars belonging to each population were combined, resulting in high signal-to-noise spectra representative of each population, which were compared to search for mean differences in Na. We find a mean abundance variation of [Na/Fe] dex for NGC 416 and [Na/Fe] dex for Lindsay 1. In both clusters we find that the population that is enhanced in N is also enhanced in Na, which is the same pattern to the one observed in ancient GCs. Furthermore, we detect a bimodal distribution of core-helium burning Red Clump (RC) giants in the UV colour magnitude diagram of NGC 416. A comparison of the stacked MUSE spectra of the two RCs shows the same mean Na abundance difference between the two populations. The results reported in this work are a crucial hint that star clusters of a large age range share the same origin: they are the same types of objects, but only separated in age
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