The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters – XVII. Public Catalogue Release

Abstract

In this paper we present the astro-photometric catalogues of 56 globular clusters and one open cluster. Astrometry and photometry are mainly based on images collected within the "HST Legacy Survey of Galactic Globular Clusters: Shedding UV Light on Their Populations and Formation" (GO-13297, PI: Piotto), and the "ACS Survey of Galactic Globular Clusters" (GO-10775, PI: Sarajedini). For each source in the catalogues for which we have reliable proper motion we also publish a membership probability for separation of field and cluster stars. These new catalogues, which we make public in Mikulski Archive for Space Telescopes, replace previous catalogues by Paper VIII of this series.PI: Sarajedini) have provided key building blocks for the observational edifice of MPs. These datasets have allowed us to demonstrate their ubiquitous presence in all Galactic GCs studied in enough details, convincingly showing the existence of discrete populations, establishing a tight connection between photometric and spectroscopic data, and spurring further studies by discovering populations with particularly complex chemical patterns (Piotto et al. 2015, hereafter Paper I;Milone et al. 2017; Marino et al. 2018 and references therein).In this paper, we present and publish the final catalogues. These catalogues contain astrometric positions, F275W, F336W, F438W, F606W, and F814W photometry and cluster membership from proper motions (PMs) of stars in the central regions of 56 GCs and the old super metalrich open cluster (OC) NGC 6791, presented in Paper I. The GO-13297 data are complemented here by the Wide Field Camera 3 (WFC3) images collected within the GO-12311 (PI: Piotto) and GO-12605 (PI: Piotto) programs, used as

The MAVERIC survey: a hidden pulsar and a black hole candidate in ATCA radio imaging of the globular cluster NGC 6397

“…Such variation is rare, so the suggested counterpart is highly likely to be the true counterpart. U97 is located fairly close (≈ 0.5 or ≈ 0.2r h ) to the cluster centre, and the suggested counterpart's proper motion matches the cluster, indicating a high membership probability (Nardiello et al 2018; Tab. 1), so U97 is very likely a cluster member.…”

“…We also incorporate results from the HST UV Globular Cluster Survey ("HUGS"; Piotto et al 2015;Nardiello et al 2018) into our analyses, which provides photometry in three HST/WFC3 bands: F275W (UV 275 ), F336W (U 336 ), F438W (B 438 ), and two HST/ACS bands: F606W (V 606 ), F814W (I 814 ). The latter are adapted from the ACS Survey of Galactic Globular Clusters (ACS GCS; GO-10775, PI: Sarajedini;Sarajedini et al 2007;Anderson et al 2008).…”

Chromosome maps of young LMC clusters: an additional case of coeval multiple populations

“…The power of such a combination comes from two aspects: 1) the colour combination (m F275W − m F814W ) on the x-axis is mostly sensitive to temperature variations, and so to He-abundance variations among different stellar populations; 2) the filter combination (m F275W − m F336W ) − (m F336W − m F438W ) = C F275W,F336W,F438W on the y-axis is mainly a measure of the N-abundance variations within the cluster. The MPs phenomenon of Galactic GCs has been extensively investigated via the chromosome map in the last years thanks to the UV Legacy Survey of Galactic GCs (Piotto et al 2015;Nardiello et al 2018). It allowed the identification of, for example, the interesting trends between the light-elements enhancement in a cluster and its total mass.…”

Another relic bulge globular cluster: ESO 456-SC38 (Djorgovski 2)

“…We made use of HST observations collected during the mission GO-14074 (PI: Cohen, mean epoch 2016.4) in F606W with the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS), and in F110W and F160W with the IR channel of the Wide Field Camera 3 (WFC3). For the data reduction we adopted the software kitchen sync2, developed by J. Anderson (Anderson et al 2008) that was also used by Nardiello et al (2018) to extract an atlas of 56 GCs. Briefly, using flc images (i.e., corrected for charge transfer inefficency, Anderson & Bedin 2010) and perturbed empirical arrays of point spread functions (PSF), the software analyzes all the exposures simultaneously to find and measure the sources.…”

“…Briefly, using flc images (i.e., corrected for charge transfer inefficency, Anderson & Bedin 2010) and perturbed empirical arrays of point spread functions (PSF), the software analyzes all the exposures simultaneously to find and measure the sources. We refer to Nardiello et al (2018) and Bellini et al (2017) for a detailed description of this approach. The magnitudes were calibrated into the Vega-mag system by comparing aperture pho- Fig.…”