The Next Generation Virgo Cluster Survey-Infrared (Ngvs-Ir). I. A New Near-Ultraviolet, Optical, and Near-Infrared Globular Cluster Selection Tool

Muñoz, Roberto P.; Puzia, Thomas H.; Lançon, A.; Peng, Eric W.; Côté, Patrick; Ferrarese, Laura; Blakeslee, John P.; Mei, S.; Cuillandre, Jean-Charles; Hudelot, P.; Courteau, Stéphane; Duc, Pierre–Alain; Balogh, Michael L.; Boselli, A.; Bournaud, F.; Carlberg, R. G.; Chapman, Scott; Durrell, Patrick R.; Eigenthaler, Paul; Emsellem, Éric; Gavazzi, G.; Gwyn, Stephen; Huertas-Company, M.; Ilbert, O.; Jordán, Andrés; Laesker, Ronald; Licitra, R.; Liu, Chengze; MacArthur, Lauren A.; McConnachie, Alan W.; McCracken, H. J.; Mellier, Y.; Peng, Chien Y.; Raichoor, Anand; Taylor, Matthew A.; Tonry, J.; Tully, R. Brent; Zhang, Hongxin

doi:10.1088/0067-0049/210/1/4

Cited by 82 publications

(72 citation statements)

References 75 publications

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“…The strongest gradients are found for u * -g within bright galaxies, inside 2.0 R e,g , while galaxies with M g > -15 have little-to-none in either color. Mild negative 4 UV and deep NIR imaging of the Virgo cluster exist (Boselli et al 2011;Muñoz et al 2014) but can only aid us for brighter galaxies and select fields, respectively. .…”

Section: The Red Sequence In the Core Of Virgomentioning

confidence: 99%

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The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼10⁶ L_⊙ and Comparisons with Galaxy Formation Models

Roediger

Ferrarese

Côté

et al. 2017

ApJ

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We use deep optical photometry from the Next Generation Virgo Cluster Survey [NGVS] to investigate the color-magnitude diagram for the galaxies inhabiting the core of this cluster. The sensitivity of the NGVS imaging allows us to continuously probe galaxy colors over a factor of ∼ 2×10 5 in luminosity, from brightest cluster galaxies to scales overlapping classical satellites of the Milky Way [M g ∼ -9; M * ∼ 10 6 M ], within a single environment. Remarkably, we find the first evidence that the RS flattens in all colors at the faint-magnitude end [starting between -14 ≤ M g ≤ -13, around M * ∼ 4 × 10 7 M ], with the slope decreasing to ∼60% or less of its value at brighter magnitudes. This could indicate that the stellar populations of faint dwarfs in Virgo's core share similar characteristics [e.g. constant mean age] over ∼3 mags in luminosity, suggesting that these galaxies were quenched coevally, likely via pre-processing in smaller hosts. We also compare our results to galaxy formation models, finding that the RS in model clusters have slopes at intermediate magnitudes that are too shallow, and in the case of semi-analytic models, do not reproduce the flattening seen at both extremes [bright/faint] of the Virgo RS. Deficiencies in the chemical evolution of model galaxies likely contribute to the model-data discrepancies at all masses, while overly efficient quenching may also be a factor at dwarf scales. Deep UV and near-IR photometry are required to unambiguously diagnose the cause of the faint-end flattening.

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Section: The Red Sequence In the Core Of Virgomentioning

confidence: 99%

“…Briefly though, GCs and UCDs were both identified via magnitude cuts and the u * ıK diagram (Muñoz et al 2014), and separated from each other through size constraints [r h ≥ 11 pc for UCDs]. The validity of candidate GCs are assessed probabilistically and we use only those having a probability > 50%.…”

Section: Comparison To Compact Stellar Systemsmentioning

confidence: 99%

The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼10⁶ L_⊙ and Comparisons with Galaxy Formation Models

Roediger

Ferrarese

Côté

et al. 2017

ApJ

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“…For example, H12 used this technique to discover 800 new GC candidates around NGC 5128 using B and R photometry. While this strategy is useful as a first guess, Muñoz et al (2014) recently showed the dramatically increased effectiveness of identifying GCs in colour-colour diagnostic space covering the NUV to near-infrared (NIR) SED range. Presently, there is no matching wide-field NIR photometry available for NGC 5128, so here we combine the u , r , and z filters from our survey which maximize the separation of GCs from background objects and, in particular, foreground stars.…”

Section: Two-colour Gc Selectionmentioning

confidence: 99%

The Survey of Centaurus A's Baryonic Structures (SCABS) – II. The extended globular cluster system of NGC 5128 and its nearby environment

Taylor

Puzia

Muñoz

et al. 2017

Monthly Notices of the Royal Astronomical Society

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New wide-field u g r i z Dark Energy Camera observations centred on the nearby giant elliptical galaxy NGC 5128 covering ∼ 21 deg 2 are used to compile a new catalogue of ∼ 3 200 globular clusters (GCs). We report 2 404 newly identified candidates, including the vast majority within ∼ 140 kpc of NGC 5128. We find evidence for a transition at a galactocentric radius of R gc ≈ 55 kpc from GCs "intrinsic" to NGC 5128 to those likely to have been accreted from dwarf galaxies or that may transition to the intragroup medium of the Centaurus A galaxy group. We fit power-law surface number density profiles of the form Σ N,Rgc ∝ R Γ gc and find that inside the transition radius, the red GCs are more centrally concentrated than the blue, with Γ inner,red ≈ −1.78 and Γ inner,blue ≈ −1.40, respectively. Outside this region both profiles flatten, more dramatically for the red GCs (Γ outer,red ≈ −0.33) compared to the blue (Γ outer,blue ≈ −0.61), although the former is more likely to suffer contamination by background sources. The median (g −z ) 0 = 1.27 mag colour of the inner red population is consistent with arising from the amalgamation of two giant galaxies each less luminous than present-day NGC 5128. Both in-and out-ward of the transition radius, we find the fraction of blue GCs to dominate over the red GCs, indicating a lively history of minormergers. Assuming the blue GCs to originate primarily in dwarf galaxies, we model the population required to explain them, while remaining consistent with NGC 5128's present-day spheroid luminosity. We find that that several dozen dwarfs of luminosities L dw,V 10 6−9.3 L V, , following a Schechter luminosity function with a faint-end slope of −1.50 α −1.25 is favoured, many of which may have already been disrupted in NGC 5128's tidal field.

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“…Muñoz et al (2014) demonstrated that incorporation of K-band photometry in color-color selections provides a much better discriminant between GCs and contaminants. There are still difficulties with identifying real GCs outside typical color-color selections.…”

Section: Ground-based Photometry and Spectroscopymentioning

confidence: 99%

THE SLUGGS SURVEY:HST/ACS MOSAIC IMAGING OF THE NGC 3115 GLOBULAR CLUSTER SYSTEM

Jennings

Strader

Romanowsky

et al. 2014

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We present Hubble Space Telescope/Advanced Camera for Surveys (HST/ACS) g and z photometry and half-light radii R h measurements of 360 globular cluster (GC) candidates around the nearby S0 galaxy NGC 3115. We also include Subaru/Suprime-Cam g, r, and i photometry of 421 additional candidates. The well-established color bimodality of the GC system is obvious in the HST/ACS photometry. We find evidence for a "blue tilt" in the blue GC subpopulation, wherein the GCs in the blue subpopulation get redder as luminosity increases, indicative of a mass-metallicity relationship. We find a color gradient in both the red and blue subpopulations, with each group of clusters becoming bluer at larger distances from NGC 3115. The gradient is of similar strength in both subpopulations, but is monotonic and more significant for the blue clusters. On average, the blue clusters have ∼10% larger R h than the red clusters. This average difference is less than is typically observed for early-type galaxies but does match that measured in the literature for the Sombrero Galaxy (M104), suggesting that morphology and inclination may affect the measured size difference between the red and blue clusters. However, the scatter on the R h measurements is large. We also identify 31 clusters more extended than typical GCs, which we term ultra-compact dwarf (UCD) candidates. Many of these objects are actually considerably fainter than typical UCDs. While it is likely that a significant number will be background contaminants, six of these UCD candidates are spectroscopically confirmed as NGC 3115 members. To explore the prevalence of low-mass X-ray binaries in the GC system, we match our ACS and Suprime-Cam detections to corresponding Chandra X-ray sources. We identify 45 X-ray-GC matches: 16 among the blue subpopulation and 29 among the red subpopulation. These X-ray/GC coincidence fractions are larger than is typical for most GC systems, probably due to the increased depth of the X-ray data compared to previous studies of GC systems.

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The Next Generation Virgo Cluster Survey-Infrared (Ngvs-Ir). I. A New Near-Ultraviolet, Optical, and Near-Infrared Globular Cluster Selection Tool

Cited by 82 publications

References 75 publications

The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼10⁶ L_⊙ and Comparisons with Galaxy Formation Models

The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼10⁶ L_⊙ and Comparisons with Galaxy Formation Models

The Survey of Centaurus A's Baryonic Structures (SCABS) – II. The extended globular cluster system of NGC 5128 and its nearby environment

THE SLUGGS SURVEY:HST/ACS MOSAIC IMAGING OF THE NGC 3115 GLOBULAR CLUSTER SYSTEM

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The Next Generation Virgo Cluster Survey-Infrared (Ngvs-Ir). I. A New Near-Ultraviolet, Optical, and Near-Infrared Globular Cluster Selection Tool

Cited by 82 publications

References 75 publications

The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼106 L⊙ and Comparisons with Galaxy Formation Models

The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼106 L⊙ and Comparisons with Galaxy Formation Models

The Survey of Centaurus A's Baryonic Structures (SCABS) – II. The extended globular cluster system of NGC 5128 and its nearby environment

THE SLUGGS SURVEY:HST/ACS MOSAIC IMAGING OF THE NGC 3115 GLOBULAR CLUSTER SYSTEM

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Product

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The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼10⁶ L_⊙ and Comparisons with Galaxy Formation Models

The Next Generation Virgo Cluster Survey (NGVS). XXIV. The Red Sequence to ∼10⁶ L_⊙ and Comparisons with Galaxy Formation Models