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doi:10.1086/529162

Cited by 25 publications

(13 citation statements)

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“…As recently pointed out by Dalessandro et al (2008), NGC 2419 contains one of the largest BSS populations ever observed in a globular cluster, with more than 230 objects found in the brightest part of the main sequence. Among them we detected one binary system and 12 pulsating variables with periods in the range from 0.041 to 0.140 d and hints, in the same cases, for the existence of several secondary periodicities.…”

Section: The Sx Phoenicis Starsmentioning

confidence: 89%

“…CMDs for the cluster were published by Christian & Heasley (1988), Harris et al (1997), Stetson (1998Stetson ( , 2005, Saha et al (2005), Sirianni et al (2005), and, more recently, by Bellazzini (2007), Ripepi et al (2007), Dalessandro et al (2008), and Sandquist & Hess (2008). Due to the large distance, the ground-based CMDs of NGC 2419 do not generally go fainter than the cluster main-sequence turnoff (TO).…”

Section: Introductionmentioning

confidence: 99%

“…Ripepi et al's (2007) CMD showed that the horizontal branch (HB) of NGC 2419 extends down to an extremely long blue tail ending with the "blue hook" for V 23.8 mag (see Brown et al 2010, for a detailed discussion of the blue hook origin in NGC 2419 and other GGCs). The cluster also has a prominent blue straggler star (BSS) sequence populated by an extraordinarily large number of BSSs (see also Dalessandro et al 2008).…”

Section: Introductionmentioning

confidence: 99%

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A New Census of the Variable Star Population in the Globular Cluster NGC 2419

Criscienzo¹,

Greco²,

Ripepi³

et al. 2011

The Astronomical Journal

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We present B, V , and I CCD light curves for 101 variable stars belonging to the globular cluster NGC 2419, 60 of which are new discoveries, based on data sets obtained at the Telescopio Nazionale Galileo, the Subaru telescope, and the Hubble Space Telescope. The sample includes 75 RR Lyrae stars (38 RRab, 36 RRc, and one RRd), one Population II Cepheid, 12 SX Phoenicis variables, two δ Scuti stars, three binary systems, five long-period variables, and three variables of uncertain classification. The pulsation properties of the RR Lyrae variables are close to those of Oosterhoff type II clusters, consistent with the low metal abundance and the cluster horizontal branch morphology, disfavoring (but not totally ruling out) an extragalactic hypothesis for the origin of NGC 2419. The observed properties of RR Lyrae and SX Phoenicis stars are used to estimate the cluster reddening and distance, using a number of different methods. Our final value is μ 0 (NGC 2419) = 19.71 ± 0.08 mag (D = 87.5 ± 3.3 kpc), with E(B − V ) = 0.08 ± 0.01 mag, [Fe/H] = −2.1 dex on the Zinn & West metallicity scale, and a value of M V that sets μ 0 (LMC) = 18.52 mag. This value is in good agreement with the most recent literature estimates of the distance to NGC 2419.

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Section: The Sx Phoenicis Starsmentioning

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A New Census of the Variable Star Population in the Globular Cluster NGC 2419

Criscienzo¹,

Greco²,

Ripepi³

et al. 2011

The Astronomical Journal

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“…Therefore, our main aim in this paper is to chart the evolving space density of mergers. Similar work has been undertaken by Lin et al (2008) and Bundy et al (2009), although these papers used pair counts to select merging galaxies, while our approach is based on morphological selection. Our analysis is thus quite complementary to Lin et al (2008) and Bundy et al (2009).…”

Section: Introductionmentioning

confidence: 98%

“…The galaxy merger rate is generally parameterized by a power law of the form (1 + z) m , and the value of the exponent of this parametric form has been used to place constraints on how much mass is assembled via major galaxy mergers. Large variations in m are found in the literature, ranging from m ∼ 0 to m ∼ 4 (Bundy et al 2004(Bundy et al , 2009Conselice et al 2003;Guo & White 2008;Lin et al 2004Lin et al , 2008Bridge et al 2007;Lotz et al 2008b;Jogee et al 2009). A recent study by Bridge et al (2010) analyzed these published merger rates and concluded that, overall, there is a general agreement that the merger rate at intermediate redshifts (0.2 < z < 1.2) does evolve, although the constraints on m remain fairly mild.…”

Section: Introductionmentioning

confidence: 99%

The Space Density Evolution of Wet and Dry Mergers in the Canada-France-Hawaii Telescope Legacy Survey

Chou¹,

Bridge²,

Abraham³

2011

The Astronomical Journal

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We analyze 1298 merging galaxies with redshifts up to z = 0.7 from the Canada-France-Hawaii Telescope Legacy Survey, taken from the catalog presented in the work of Bridge et al. By analyzing the internal colors of these systems, we show that the so-called wet and dry mergers evolve in different senses, and quantify the space densities of these systems. The local space density of wet mergers is essentially identical to the local space density of dry mergers. The evolution in the total merger rate is modest out to z ∼ 0.7, although the wet and dry populations have different evolutionary trends. At higher redshifts, dry mergers make a smaller contribution to the total merging galaxy population, but this is offset by a roughly equivalent increase in the contribution from wet mergers. By comparing the mass density function of early-type galaxies to the corresponding mass density function for merging systems, we show that not all the major mergers with the highest masses (M stellar > 10 11 M ) will end up with the most massive early-type galaxies, unless the merging timescale is dramatically longer than that usually assumed. On the other hand, the usually assumed merging timescale of ∼0.5-1 Gyr is quite consistent with the data if we suppose that only less massive early-type galaxies form via mergers. Since low-intermediate-mass ellipticals are 10-100 times more common than their most massive counterparts, the hierarchical explanation for the origin of early-type galaxies may be correct for the vast majority of early types, even if incorrect for the most massive ones.

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A guided map to the spiral arms in the galactic disk of the Milky Way

Vallée

2017

Astronomical Review

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An up-to-date overview of the recent history is given, aiming is to present a helpful working guide to the literature and at the same time introduce key systems and observational results, starting from the Sun and going toward the Galactic Center and parts of the Zona Galactica Incognita, and beyond. We start by presenting an observational view of the Milky Way's disk plane (cartographic, dynamical, chemical crosscut, magnetic). This included the four long spiral arms in the disk of the Milky Way galaxy, their geometry, components, velocity, their widths and internal layers as well as onion-like ordered offsets, the central galactic bars, arm tangents, arm pitch and arm shape, arm origins near the Galactic Center, and other possible players in the spiral arm, such as the magnetic field and the dark matter content. After, we present a basic analysis of some theoretical predictions from galactic arm formation: numerical simulations or analytical theories, and observations are checked against predictions from various numerical simulations and analytical (theoretical) models.

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Cited by 25 publications

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A New Census of the Variable Star Population in the Globular Cluster NGC 2419

A New Census of the Variable Star Population in the Globular Cluster NGC 2419

The Space Density Evolution of Wet and Dry Mergers in the Canada-France-Hawaii Telescope Legacy Survey

A guided map to the spiral arms in the galactic disk of the Milky Way

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