A MUSE study of the inner bulge globular cluster Terzan 9: a fossil record in the Galaxy

Ernandes, H.; Dias, B.; Barbuy, B.; Kamann, Sebastian; Ortolani, S.; Cantelli, E.; Bica, E.; Rossi, Luca

doi:10.1051/0004-6361/201936431

Cited by 11 publications

(14 citation statements)

References 50 publications

(100 reference statements)

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“…We note that the optical results from Ernandes et al (2019) actually appear quite bimodal, with a peak near -1.4 and another near -0.7, with the former agreeing with our value. Given their mean metallicity of -1.1, and the relatively blue HB suggested by the ground-based optical CMD of Ortolani et al (1999), they found Terzan 9 to be a good candidate for a very old GC.…”

Section: Metallicitysupporting

confidence: 90%

“…In addition, from the same DR16 ASPCAP database and for the same sample of stars as ours, Kunder & Butler (2020) derive [Si/Fe] = 0.25 for Djorg 2, 0.04 dex lower than our value, again as expected given their inclusion of 2G stars. Ernandes et al (2019) derive [Mg/Fe] = 0.27±0.03 for Terzan 9 from low-resolution optical spectra, in accord with our value of 0.22±0.03. A comparison with the only other independent high-resolution studies, including other elements besides αs, will be described in more detail below.…”

Section: The α-Elementssupporting

confidence: 90%

“…No other high-resolution abundance study has been carried out. Among the most reliable studies are those of Dias et al (2016), who found -1.06±0.13 from low-resolution optical spectra, the Ernandes et al (2019) value of -1.10±0.15, also from low-resolution optical as well as near-IR spectra, and several studies using the CaT technique, including Vásquez et al (2018), who yield values ranging from -1.08 to -1.21 depending on their calibration, and Geisler et al (2021), who give -1.12±0.03. Our value is in relatively poor agreement with both H10 and most of the low-resolution spectroscopic studies, falling to lower metallicity than all of them.…”

Section: Metallicitymentioning

confidence: 99%

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CAPOS: The bulge Cluster APOgee Survey

Geisler

Villanova

O’Connell

et al. 2021

A&A

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Context. Bulge globular clusters (BGCs) are exceptional tracers of the formation and chemodynamical evolution of this oldest Galactic component. However, until now, observational difficulties have prevented us from taking full advantage of these powerful Galactic archeological tools. Aims. CAPOS, the bulge Cluster APOgee Survey, addresses this key topic by observing a large number of BGCs, most of which have only been poorly studied previously. Even their most basic parameters, such as metallicity, [α/Fe], and radial velocity, are generally very uncertain. We aim to obtain accurate mean values for these parameters, as well as abundances for a number of other elements, and explore multiple populations. In this first paper, we describe the CAPOS project and present initial results for seven BGCs. Methods. CAPOS uses the APOGEE-2S spectrograph observing in the H band to penetrate obscuring dust toward the bulge. For this initial paper, we use abundances derived from ASPCAP, the APOGEE pipeline. Results. We derive mean [Fe/H] values of −0.85 ± 0.04 (Terzan 2), −1.40 ± 0.05 (Terzan 4), −1.20 ± 0.10 (HP 1), −1.40 ± 0.07 (Terzan 9), −1.07 ± 0.09 (Djorg 2), −1.06 ± 0.06 (NGC 6540), and −1.11 ± 0.04 (NGC 6642) from three to ten stars per cluster. We determine mean abundances for eleven other elements plus the mean [α/Fe] and radial velocity. CAPOS clusters significantly increase the sample of well-studied Main Bulge globular clusters (GCs) and also extend them to lower metallicity. We reinforce the finding that Main Bulge and Main Disk GCs, formed in situ, have [Si/Fe] abundances slightly higher than their accreted counterparts at the same metallicity. We investigate multiple populations and find our clusters generally follow the light-element (anti)correlation trends of previous studies of GCs of similar metallicity. We finally explore the abundances of the iron-peak elements Mn and Ni and compare their trends with field populations. Conclusions. CAPOS is proving to be an unprecedented resource for greatly improving our knowledge of the formation and evolution of BGCs and the bulge itself.

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Section: Metallicitysupporting

confidence: 90%

Section: The α-Elementssupporting

confidence: 90%

Section: Metallicitymentioning

confidence: 99%

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CAPOS: The bulge Cluster APOgee Survey

Geisler

Villanova

O’Connell

et al. 2021

A&A

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“…Furthermore, recent studies have demonstrated that some other luminous GCs may be actually arXiv:2103.03592v1 [astro-ph.GA] 5 Mar 2021 A&A proofs: manuscript no. newGCs_v28 fossil relics of accreted dwarf galaxies, such as Terzan 5 (Ferraro et al 2009), Liller 1 (Ferraro et al 2020), Terzan 9 (Ernandes et al 2019) and also Omega Centauri (Lee et al 1999;Sollima et al 2008). Further, with the advent of Gaia Mission and deep surveys, it is now possible to associate individual GCs with specific merger events (e.g., Vasiliev 2019;Myeong et al 2019;Massari et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Confirmation and physical characterization of the new bulge globular cluster Patchick 99 from the VVV and Gaia surveys

Garro

Minniti

Gómez

et al. 2021

A&A

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Context. Globular clusters (GCs) are recognised as important tools for understanding the formation and evolution of the Milky Way (MW) because they are the oldest objects in our Galaxy. Unfortunately, the known sample in our MW is still incomplete, especially towards the innermost regions, because of the high differential reddening, extinction, and stellar crowding. Therefore, the discovery of new GC candidates and the confirmation of their true nature are crucial for the census of the MW GC system. Aims. Our main goal is to confirm the physical nature of two GC candidates: Patchick 99 and TBJ 3. Both are located towards the Galactic bulge. We use public data in the near-infrared(IR) passband from the VISTA Variables in the Via Láctea Survey (VVV), the VVV eXtended Survey, and the Two Micron All Sky Survey along with deep optical data from the Gaia Mission DR 2 in order to estimate their main astrophysical parameters, such as reddening and extinction, distance, total luminosity, mean cluster proper motions, size, metallicity, and age. Methods. We investigated both candidates at different wavelengths, allowing us to discard TBJ3 as a possible GC. We use near-IR (Ks vs. (J − Ks)) and optical (G vs. (BP − RP)) colour–magnitude diagrams (CMDs) in order to analyse Patchick 99. First, we decontaminated CMDs, following a statistical procedure, as well as selecting only stars which have similar proper motions (PMs) and are situated within 3′ of the centre. Mean PMs were measured from Gaia DR 2 data. Reddening and extinction were derived by adopting optical and near-IR reddening maps, and were used to estimate the distance modulus and the heliocentric distance. Metallicity and age were evaluated by fitting theoretical stellar isochrones. Results. Reddening and extinction values for Patchick 99 are E(J − Ks) = (0.12 ± 0.02) mag and AKs = (0.09 ± 0.01) mag from the VVV data, whereas we calculate E(BP − RP) = (0.21 ± 0.03) mag and AG = (0.68 ± 0.08) mag from Gaia DR 2 data. We use those values and the magnitude of the RC to estimate the distance, finding good agreement between the near-IR and optical measurements. In fact, we obtain (m − M)0 = (14.02 ± 0.01) mag, equivalent to a distance D = (6.4 ± 0.2) kpc in near-IR and (m − M)0 = (14.23 ± 0.1) mag and so D = (7.0 ± 0.2) kpc in optical. In addition, we derive the metallicity and age for Patchick 99 using our distance and extinction values and fitting PARSEC isochrones. We find [Fe/H]=(−0.2 ± 0.2) dex and t = (10 ± 2) Gyr. The mean PMs for Patchick 99 are μα = ( − 2.98 ± 1.74) mas yr−1 and μδ = ( − 5.49 ± 2.02) mas yr−1 using the Gaia DR 2 data. These are consistent with the bulge kinematics. We also calculate the total luminosity of our cluster and confirm that it is a low-luminosity GC, with MKs = ( − 7.0 ± 0.6) mag. The radius estimation is performed building the radial density profile and we find its angular radius rP99 ∼ 10′. We also recognise seven RR Lyrae star members within 8.2 arcmin from the Patchick 99 centre, but only three of them have PMs matching the mean GC PM, confirming the distance found by other methods. Conclusions. We find that TBJ 3 shows mid-IR emissions that are not present in GCs. We therefore discard TBJ 3 as a GC candidate and focus our work on Patchick 99. We conclude that Patchick 99 is an old metal-rich GC situated in the Galactic bulge. TBJ 3 is a background galaxy.

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“…This technique has been applied to several GCs and has led to the study of thousands of stars in such environments, e.g. NGC 6397 [74]; Kamann et al 2016 [75]), NGC 2808 (Latour et al 2019 [76]), NGC 3201 (Giesers et al 2018 [77]; 2019 [78]), Terzan 9 (Ernandes et al 2019 [79]), 47 Tuc (Kamann et al 2018 [80]). More recently, MUSE has been used to observe 26 GCs to identify emission-line sources, which has led to the confirmation of five CVs and the discovery of two more (Göttgens et al 2019b [71]).…”

Section: Pos(golden2019)013mentioning

confidence: 99%

Properties of Cataclysmic Variables in Globular Clusters

Belloni¹,

Rivera²

2021

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects v — PoS(GOLDEN2019)

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The study of star clusters plays an important role in our understanding of the Universe since these systems are natural laboratories for testing theories of stellar dynamics and evolution. Particularly, globular clusters (GCs) are one of the most important objects for studying the formation and the physical nature of exotic systems which in turn provide basic information and tools that can help us to understand the formation and evolution processes of star clusters themselves, galaxies and, in general, the young Universe. Among the most interesting objects in GCs are the cataclysmic variables (CVs), which are interacting binaries harbouring a white dwarf accreting from a lowmass companion. Since GC densities are sufficiently high that dynamical encounters involving binaries should be common, CV progenitors are expected to be affected by dynamics in some way in the early stages. In this article we review the formation channels and the influence of dynamics on the CV population in GCs. In particular, we review recent progress in numerical simulations. Furthermore, we discuss observational properties of CVs in GCs and the techniques used to identify and study them. We focus the discussion on the multi-wavelength observations carried out with HST and Chandra on the best-studied GCs NGC 6397, NGC 6752, 47 Tucanae and ω Centauri; on the recent spectroscopic findings with MUSE, and on updates regarding the correlation between the number of faint X-ray sources and the cluster stellar encounter rate. Finally, we discuss some observational prospects that might potentially help future investigations.

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A MUSE study of the inner bulge globular cluster Terzan 9: a fossil record in the Galaxy

Cited by 11 publications

References 50 publications

CAPOS: The bulge Cluster APOgee Survey

CAPOS: The bulge Cluster APOgee Survey

Confirmation and physical characterization of the new bulge globular cluster Patchick 99 from the VVV and Gaia surveys

Properties of Cataclysmic Variables in Globular Clusters

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