Gemini Spectroscopic Survey of Young Star Clusters in Merging/Interacting Galaxies. I. NGC 3256 Tidal Tail Clusters

Trancho, Gelys; Bastian, N.; Schweizer, F.; Miller, Bryan W.

doi:10.1086/511735

Cited by 33 publications

(30 citation statements)

References 45 publications

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“…The tail structure here in the binary system resembles the tidal tails of interacting galaxies, e.g. NGC 3256 and NGC 5752/4 (Keel & Borne 2003;Trancho et al 2007;Smith et al 2010), etc. The loosely bound tail material could get stripped during the interaction process.…”

Section: Binary Molecular Clumpmentioning

confidence: 90%

Interaction Between the Supernova Remnant Hb 3 and the Nearby Star-Forming Region W3

Zhou

Yang

Fang

et al. 2016

ApJ

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We performed millimeter observations in CO lines toward the supernova remnant (SNR) HB 3. Substantial molecular gas around −45 km s −1 is detected in the conjunction region between the SNR HB 3 and the nearby W3 complex. This molecular gas is distributed along the radio continuum shell of the remnant. Furthermore, the shocked molecular gas indicated by line wing broadening features is also distributed along the radio shell and inside it. By both morphological correspondence and dynamical evidence, we confirm that the SNR HB 3 is interacting with the −45 km s −1 molecular cloud (MC), in essence, with the nearby H ii region/MC complex W3. The red-shifted line wing broadening features indicate that the remnant is located at the nearside of the MC. With this association, we could place the remnant at the same distance as the W3/W4 complex, which is 1.95 ± 0.04 kpc. The spatial distribution of aggregated young stellar object candidates (YSOc) shows a correlation to the shocked molecular strip associated with the remnant. We also find a binary clump of CO at (l = 132• .94, b = 1 • .12) around −51.5 km sinside the projected extent of the remnant, and it is associated with significant mid-infrared (mid-IR) emission. The binary system also has a tail structure resembling the tidal tails of interacting galaxies. According to the analysis of CO emission lines, the larger clump in this binary system is about stable, and the smaller clump is significantly disturbed.

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Section: Binary Molecular Clumpmentioning

confidence: 90%

Interaction Between the Supernova Remnant Hb 3 and the Nearby Star-Forming Region W3

Zhou

Yang

Fang

et al. 2016

ApJ

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“…Scoville et al 1998; Wilson et al 2006) and NGC 3256 (e.g. Zepf et al 1999; Trancho et al 2007b) have SFRs of a few tens to hundreds of solar masses per year, and due to their proximity, can be resolved with Hubble Space Telescope imaging. In these systems large numbers of superstar clusters are often found, with ages of a 1–500 Myr and masses up to ∼8 × 10 7 M ⊙ (Maraston et al 2004).…”

Section: Introductionmentioning

confidence: 99%

On the fraction of star clusters surviving the embedded phase

Goddard

Bastian

Kennicutt

2010

Monthly Notices of the Royal Astronomical Society

144

258

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In this paper we derive ages and masses for 276 clusters in the merger galaxy NGC 3256. This was achieved by taking accurate photometry in four wavebands from archival Hubble Space Telescope images. Photometric measurements are compared to synthetic stellar population (SSP) models to find the most probable age, mass and extinction. The cluster population of NGC 3256 reveals an increase in the star formation rate (SFR) over the last 100 Myr and the initial cluster mass function (ICMF) is best described by a power‐law relation with slope α= 1.85 ± 0.12. Using the observed cluster population for NGC 3256 we calculate the implied mass of clusters younger than 10‐Myr old, and convert this to a cluster formation rate over the last 10 Myr. Comparison of this value with the SFR indicates the fraction of stars found within bound clusters after the embedded phase of cluster formation, Γ, is 22.9 ±7.39.8 per cent for NGC 3256. We carried out an in‐depth analysis into the errors associated with such calculations showing that errors introduced by the SSP fitting must be taken into account and an unconstrained metallicity adds to these uncertainties. Observational biases should also be considered. Using published cluster population data sets we calculate Γ for six other galaxies and examine how Γ varies with environment. We show that Γ increases with the SFR density and can be described as a power‐law type relation of the form Γ (per cent) = (29.0 ± 6.0) Σ0.24±0.04SFR (M ⊙ yr−1 kpc−2).

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“…By using both techniques, we are able to obtain information for a large number of clusters and also overcome the degeneracy between age and extinction that presents a hurdle in the analysis of photometric data ( Trancho et al 2007a( Trancho et al , 2007b. In this paper, we present optical spectroscopy for seven clusters that was obtained with the Gemini North 8.1 m telescope, and in a companion paper ), we present new HST imaging, including U-band photometry of the clusters.…”

Section: Introductionmentioning

confidence: 99%

Gemini Spectroscopy andHSTImaging of the Stellar Cluster Population in Region B of M82

Konstantopoulos

Bastian

Smith

et al. 2008

ApJ

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We present new spectroscopic observations of the stellar cluster population of region B in the prototype starburst galaxy M82 obtained with the Gemini North 8.1 m telescope. By coupling the spectroscopy with UBVI photometry acquired with the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope (HST ), we derive ages, extinctions, and radial velocities for seven young massive clusters (YMCs) in region B. We find the clusters to have ages between 80 and 200 Myr and velocities in the range 230Y350 km s À1 , while the extinctions A V vary between $1 and 2.5 mag. We also find evidence of differential extinction across the faces of some clusters, which hinders the photometric determination of ages and extinctions in these cases. The cluster radial velocities indicate that the clusters are located at different depths within the disk and are on regular disk orbits. Our results overall contradict the findings of previous studies, in which region B was thought to be a bound region populated by intermediate-age clusters that formed in an independent, offset starburst episode that commenced 600 MyrY1 Gyr ago. Our findings instead suggest that region B is optically bright because of low-extinction patches, and that this allows us to view the cluster population of the inner M82 disk, which probably formed as a result of the last encounter with M81. This study forms part of a series of papers whose aim is to study the cluster population of M82 using deep optical spectroscopy and multiband photometry.

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Gemini Spectroscopic Survey of Young Star Clusters in Merging/Interacting Galaxies. I. NGC 3256 Tidal Tail Clusters

Cited by 33 publications

References 45 publications

Interaction Between the Supernova Remnant Hb 3 and the Nearby Star-Forming Region W3

Interaction Between the Supernova Remnant Hb 3 and the Nearby Star-Forming Region W3

On the fraction of star clusters surviving the embedded phase

Gemini Spectroscopy andHSTImaging of the Stellar Cluster Population in Region B of M82

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