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

Minniti, D.; Dias, B.; Gómez, M.; Palma, Tali; Pullen, Joyce

doi:10.3847/2041-8213/ab4424

Cited by 13 publications

(9 citation statements)

References 66 publications

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“…We note that VVV-CL160 is also interesting because there are three candidate planetary nebulae (PNe) in the vicinity: the closest one is PHR J1806−1956 at 4.6 north of the GC center; then there are PN PM 1−209 and IRAS 18036−1954 at 4.9 west and 5.2 northwest from the center, respectively. Their membership in the GC is unknown; determining this membership spectroscopically would be significant as there are a very limited number of GC PNe known in our Galaxy (Minniti et al 2019). Of these three PNe, as far as we know only IRAS 18036−1954 has an estimated distance measurement, D = 1.67 kpc (Ortiz 2013), that is smaller than our distance determination for VVV-CL160.…”

Section: Confirmation Of a New Globular Clustermentioning

confidence: 62%

Discovery of a new nearby globular cluster with extreme kinematics located in the extension of a halo stream

Minniti

Fernández-Trincado

Gómez

et al. 2021

A&A

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Context. We report the discovery of VVV-CL160, a new nearby globular cluster (GC) with extreme kinematics, located in the Galactic plane at l = 10.1477 deg, b = 0.2999 deg. Aims. We aim to characterize the physical properties of this new GC and place it in the context of the Milky Way, exploring its possible connection with the known GC NGC 6544 and with the Hrid halo stream. Methods. VVV-CL160 was originally detected in the VISTA Variables in the Vía Láctea (VVV) survey. We use the proper motions (PMs) from the updated VVV Infrared Astrometric Catalog (VIRAC2) to select GC members and make deep near-infrared color-magnitude diagrams to study the cluster properties. We also fit King models to the decontaminated sample to determine the GC structural parameters. Results. VVV-CL160 has an unusually large PM for a Galactic GC as measured with VIRAC2 and Gaia EDR3: μα cos (δ) = −2.3 ± 0.1 mas yr−1 and μδ = −16.8 ± 0.1 mas yr−1. The kinematics are similar to those of the known GC NGC 6544 and the Hrid halo stream. We estimate a reddening of E(J − K) = 1.95 mag and an extinction of AK = 1.40 mag for VVV-CL160. We also measure a distance modulus of (m − M) = 13.01 mag and a distance of D⊙ = 4.0 ± 0.5 kpc. This places the GC at z = 29 pc above the Galactic plane and at a galactocentric distance of RG = 4.2 kpc. We also measure a metallicity of [Fe/H] = −1.4 ± 0.2 dex for an adopted age of t = 12 Gyr; King model fits of the PM-decontaminated sample reveal a concentrated GC, with core radius rc = 22.8″ and tidal radius rt = 50′. We also estimate the absolute magnitude in the near-infrared of MK = −7.6 mag, equivalent to an optical absolute magnitude of MV = −5.1 mag. We also explore the possible association of this new GC with other GCs and halo streams. Conclusions. Based on the locations and kinematics, we suggest that VVV-CL160, along with NGC 6544, may be associated with the extension of the Hrid halo stream.

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Section: Confirmation Of a New Globular Clustermentioning

confidence: 62%

Discovery of a new nearby globular cluster with extreme kinematics located in the extension of a halo stream

Minniti

Fernández-Trincado

Gómez

et al. 2021

A&A

Self Cite

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“…The Milky Way contains around 160 known GCs, although Minniti et al (2019) have reported an additional 50 GC candidates in the direction of the Milky Way's bulge. The recent compilation of K19 lists 96 GCs with ages and metallicities taken from three large studies.…”

Section: The Milky Way Gc Systemmentioning

confidence: 99%

Reverse engineering the Milky Way

Forbes

2020

Monthly Notices of the Royal Astronomical Society

145

100

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The ages, metallicities, alpha-elements and integrals of motion of globular clusters (GCs) accreted by the Milky Way from disrupted satellites remain largely unchanged over time. Here we have used these conserved properties in combination to assign 76 GCs to 5 progenitor satellite galaxies -one of which we dub the Koala dwarf galaxy. We fit a leaky-box chemical enrichment model to the age-metallicity distribution of GCs, deriving the effective yield and the formation epoch of each satellite. Based on scaling relations of GC counts we estimate the original halo mass, stellar mass and mean metallicity of each satellite. The total stellar mass of the 5 accreted satellites contributed around 10 9 M in stars to the growth of the Milky Way but over 50% of the Milky Way's GC system. The 5 satellites formed at very early times and were likely accreted 8-11 Gyr ago, indicating rapid growth for the Milky Way in its early evolution. We suggest that at least 3 satellites were originally nucleated, with the remnant nucleus now a GC of the Milky Way. Eleven GCs are also identified as having formed ex-situ but could not be assigned to a single progenitor satellite.

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“…At the other extreme, if we scale the expected number from the stellar halo in Moe & De Marco (2006), the number of PNe decreases by a factor of ∼ 10 2 due to older ages of the system (a relatively shorter dissipation timescale of stellar envelopes), but this estimate is quite uncertain. On the observational ground, however, there are 8 PNe known in the Galactic globular clusters (Jacoby et al 1997;Minniti et al 2019), from which one can naively expect ∼ 10 3 PNe since the nuclear bulge is ∼ 100 times more massive than the entire globular cluster system in the Milky Way.…”

Section: Discussion and Summarymentioning

confidence: 99%

“…On the other hand, if the observed lack of PNe is rooted in astrophysical origins, this may indicate that the PN formation channel such as binary interactions (e.g., Minniti et al 2019) is overpowered by suppression mechanisms that can reduce the envelope mass of asymptotic giant branch (AGB) stars. Some stars can also skip the AGB phase and directly evolve into hot subdwarfs, if the envelope mass is not high enough.…”

Section: Discussion and Summarymentioning

confidence: 99%

Hunting for Planetary Nebulae toward the Galactic Center

Hong,

Simpson,

et al. 2021

Preprint

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We present near-infrared (IR) spectra of two planetary nebula (PN) candidates in close lines of sight toward the Galactic center (GC) using GNIRS at Gemini North. High-resolution images from radio continuum and narrow-band IR observations reveal ring-like morphologies of these objects, and their mid-IR spectra from the Spitzer Space Telescope exhibit rich emission lines from highly excited species such as [S IV], [Ne III], [Ne V], and [O IV]. We also derive elemental abundances using the Cloudy synthetic models, and find an excess amount of the s-process element Krypton in both targets, which supports their nature as PNe. We estimate foreground extinction toward each object using near-IR hydrogen recombination lines, and find significant visual extinctions (A V > 20). The distances inferred from the size versus surface brightness relation of other PNe are 9.0 ± 1.6 kpc and 7.6 ± 1.6 kpc for SSTGC 580183 and SSTGC 588220, respectively. These observed properties along with abundance patterns and their close proximity to Sgr A * (projected distances 20 pc) make it highly probable that these objects are the first confirmed PNe objects in the nuclear stellar disk. The apparent scarcity of such objects resembles the extremely low rate of PN formation in old stellar systems, but is in line with the current rate of the sustained star formation activity in the Central Molecular Zone.

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

Cited by 13 publications

References 66 publications

Discovery of a new nearby globular cluster with extreme kinematics located in the extension of a halo stream

Discovery of a new nearby globular cluster with extreme kinematics located in the extension of a halo stream

Reverse engineering the Milky Way

Hunting for Planetary Nebulae toward the Galactic Center

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