Analysis of the physical nature of 22 New VVV Survey Globular Cluster candidates in the Milky Way bulge

Palma, Tali; Minniti, D.; Alonso-García, J.; Crestani, Juliana; Netzel, H.; Clariá, J. J.; Saito, R. K.; Dias, B.; Fernández-Trincado, J. G.; Kammers, R.; Geisler, D.; Gómez, M.; Hempel, M.; Pullen, Joyce

doi:10.1093/mnras/stz1489

Cited by 46 publications

(46 citation statements)

References 59 publications

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“…We used different tracers, such as RR Lyrae, type 2 Cepheids, red clump (RC) giants, and blue horizontal branch (BHB) stars, uncovering more than 300 new candidates (e.g., Camargo & Minniti 2019;Palma et al 2019;Montenegro et al 2019;Barba et al 2019;Minniti et al 2020 and references therein). As the Sgr dwarf galaxy is projected behind the Galactic bulge, it is not surprising to expect that some of these new candidate GCs may belong to this galaxy.…”

Section: Introductionmentioning

confidence: 99%

Discovery of new globular clusters in the Sagittarius dwarf galaxy

Minniti

Ripepi

Fernández-Trincado

et al. 2021

A&A

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Context. Globular clusters (GCs) are witnesses of the past accretion events onto the Milky Way. In particular, the GCs of the Sagittarius (Sgr) dwarf galaxy are important probes of an on-going merger. Aims. Our main goal is to search for new GC members of this dwarf galaxy using the VISTA Variables in the Via Lactea Extended Survey (VVVX) near-infrared database combined with the Gaia Early Data Release 3 (EDR3) optical database. Methods. We investigated all VVVX-enabled discoveries of GC candidates in a region covering about 180 sq. deg. toward the bulge and the Sgr dwarf galaxy. We used multiband point-spread function photometry to obtain deep color-magnitude diagrams (CMDs) and luminosity functions (LFs) for all GC candidates, complemented by accurate Gaia-EDR3 proper motions (PMs) to select Sgr members and variability information to select RR Lyrae which are potential GC members. Results. After applying a strict PM cut to discard foreground bulge and disk stars, the CMDs and LFs for some of the GC candidates exhibit well defined red giant branches and red clump giant star peaks. We selected the best Sgr GCs, estimating their distances, reddenings, and associated RR Lyrae. Conclusions. We discover 12 new Sgr GC members, more than doubling the number of GCs known in this dwarf galaxy. In addition, there are 11 other GC candidates identified that are uncertain, awaiting better data for confirmation.

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Section: Introductionmentioning

confidence: 99%

Discovery of new globular clusters in the Sagittarius dwarf galaxy

Minniti

Ripepi

Fernández-Trincado

et al. 2021

A&A

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“…3.3. PN G356.8-03.6 in the GC Minni 28 Field Minni 28 is classified as a metal-poor GC, and appears to be located in the far side of the bulge, at D = 10.1 ± 1.5 kpc (Palma et al 2019).…”

Section: Pn Sb 2 In the Gc Minni 06 Fieldmentioning

confidence: 99%

“…The GC Minni 31 is also metal-poor, and located in the bulge at D = 9.1 ± 1.5 kpc (Palma et al 2019). PN Pe 2-11 (a.k.a.…”

Section: Pn Pe 2-11 In the Gc Minni 31 Fieldmentioning

confidence: 99%

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New Candidate Planetary Nebulae in Galactic Globular Clusters from the VVV Survey*

Minniti

Dias

Gómez

et al. 2019

ApJL

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Only four globular cluster planetary nebulae (GCPN) are known so far in the Milky Way. About 50 new globular clusters have been recently discovered towards the Galactic bulge. We present a search for planetary nebulae within 3 arcmin of the new globular clusters, revealing the identification of new candidate GCPN. These possible associations are PN SB 2 with the GC Minni 06, PN G354.9-02.8 with the GC Minni 11, PN G356.8-03.6 with the GC Minni 28, and PN Pe 2-11 with the GC Minni 31. We discard PN H 2-14 located well within the projected tidal radius of the new globular cluster FSR1758 because they have different measured radial velocities. These are interesting objects that need follow-up observations (especially radial velocities) in order to confirm membership, and to measure their physical properties in detail. If confirmed, this would double the total number of Galactic GCPN.

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“…This census is expected to increase -especially towards the faint end of the GC distribution, as deep photometric surveys become available. For instance, working with photometry from the VISTA Infrared Camera (VIRCAM -Emerson & Sutherland 2010) at the 4m VISTA telescope at the ESO Cerro Paranal Observatory, Palma et al (2019) present 17 new candidates to Bulge GCs. Having being formed -or accreted -at the early stages of the Galaxy, determining the present-day parameters of all the individual GCs, together with their large-scale spatial distribution, may provide important clues to the Milky Way assembly process as well as to the chemical and physical conditions then prevailing.…”

Section: Introductionmentioning

confidence: 99%

Lifting the dust veil from the globular cluster Palomar 2

Bonatto

Chies-Santos

2020

Monthly Notices of the Royal Astronomical Society

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This work employs high-quality Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) F606W and F814W photometry to correct for the differential reddening affecting the colour-magnitude diagram (CMD) of the poorly-studied globular cluster (GC) Palomar 2. Differential reddening is taken into account by assuming that morphological differences among CMDs extracted across the field of view of Palomar 2 correspond essentially to shifts (quantified in terms of δE(B − V )) along the reddening vector due to a non-uniform dust distribution. The average reddening difference over all partial CMDs is δE(B − V ) = 0.24 ± 0.08, with the highest reaching δE(B − V ) = 0.52. The corrected CMD displays well-defined and relatively narrow evolutionary sequences, especially for the evolved stars, i.e. the red-giant, horizontal and asymptotic giant branches (RGB, HB and AGB, respectively). The average width of the upper main sequence and RGB profiles of the corrected CMD corresponds to 56% of the original one. Parameters measured on this CMD show that Palomar 2 is ≈ 13.25 Gyr old, has the mass M ∼ 1.4 × 10 5 M stored in stars, is affected by the foreground E(B − V ) ≈ 0.93, is located at d ≈ 26 Kpc from the Sun, and is characterized by the global metallicity Z/Zo ≈ 0.03, which corresponds to the range −1.9 ≤ [F e/H] ≤ −1.6 (for 0.0 ≤ [α/F e] ≤ +0.4), quite consistent with other outer halo GCs. Additional parameters are the absolute magnitude M V ≈ −7.8, and the core and half-light radii r C ≈ 2.6 pc and R HL ≈ 4.7 pc, respectively.

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Analysis of the physical nature of 22 New VVV Survey Globular Cluster candidates in the Milky Way bulge

Cited by 46 publications

References 59 publications

Discovery of new globular clusters in the Sagittarius dwarf galaxy

Discovery of new globular clusters in the Sagittarius dwarf galaxy

New Candidate Planetary Nebulae in Galactic Globular Clusters from the VVV Survey*

Lifting the dust veil from the globular cluster Palomar 2

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