Paul, Founder of Churches

Barentsen, Jack

doi:10.1163/25890468-058-02-90000014

Cited by 16 publications

(36 citation statements)

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“…Their work is mainly based on photometric observations from the "Coordinated Synoptic Investigation of NGC 2264" (CSI) 2264 project (Cody et al 2014) in combination with data from other photometric and spectroscopic observational campaigns (e.g. SDSS, Gaia-ESO, IPHAS, Pan-STARRS1, Abazajian et al 2009;Randich et al 2013;Barentsen et al 2014;Flewelling et al 2020).…”

Section: Observational Datamentioning

confidence: 99%

Constraints on star formation in NGC 2264

Parker

Schoettler

2021

Monthly Notices of the Royal Astronomical Society

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We quantify the spatial distribution of stars for two subclusters centred around the massive/intermediate mass stars S Mon and IRS 1/2 in the NGC 2264 star-forming region. We find that both subclusters are have neither a substructured, nor a centrally concentrated distribution according to the $\mathcal {Q}$-parameter. Neither subcluster displays mass segregation according to the ΛMSR ratio, but the most massive stars in IRS 1/2 have higher relative surface densities according to the ΣLDR ratio. We then compare these quantities to the results of N-body simulations to constrain the initial conditions of NGC 2264, which are consistent with having been dense ($\tilde{\rho } \sim 10^4$ M⊙ pc−3), highly substructured and subvirial. These initial conditions were also derived from a separate analysis of the runaway and walkaway stars in the region, and indicate that star-forming regions within 1 kpc of the Sun likely have a broad range of initial stellar densities. In the case of NGC 2264, its initial stellar density could have been high enough to cause the destruction or truncation of protoplanetary discs and fledgling planetary systems due to dynamical encounters between stars in the early stages of its evolution.

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Section: Observational Datamentioning

confidence: 99%

Constraints on star formation in NGC 2264

Parker

Schoettler

2021

Monthly Notices of the Royal Astronomical Society

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“…In these instances, coordinates from SIMBAD were used instead (Wenger et al 2000, accessed on 23/05/2018). We checked the coordinates for accuracy using images from VPHAS+ DR3 (Drew et al 2014), IPHAS DR2 (Barentsen et al 2014, Drew et al 2005 and 2MASS (Skrutskie et al 2006), to ensure they corresponded to isolated WR stars. The remaining 243 WR stars yielded no successful results with either coordinate set.…”

Section: Gaia Dr2 Cataloguementioning

confidence: 99%

Unlocking Galactic Wolf-Rayet stars with $\textit{Gaia}$ DR2 I: Distances and absolute magnitudes

Rate,

Crowther

2019

Preprint

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We obtain distances to 383 Galactic Wolf-Rayet (WR) stars from Gaia DR2 parallaxes and Bayesian methods, with a prior based on HII regions and dust extinction. Distances agree with those from Bailer-Jones et al. for stars up to 2 kpc from the Sun, though deviate thereafter due to differing priors, leading to modest reductions in luminosities for recent WR spectroscopic results. We calculate visual and K-band absolute magnitudes, accounting for dust extinction contributions and binarity, and identify 187 stars with reliable absolute magnitudes. For WR and O stars within 2 kpc, we find a WR/O ratio of 0.09. The distances are used to generate absolute magnitude calibrations and obtain the Gaia colour magnitude diagram for WR stars. Average v WR -band absolute magnitudes for WN stars range from -3.6 mag (WN3-4) to -7.0 mag (WN8-9ha), and -3.1 (WO2-4) to -4.6 mag (WC9), with standard deviations of ∼0.6 mag. Using HII region scale heights, we identify 31 WR stars at large (3σ, |z|≥156 pc) distances from the mid-plane as potential runaways accounting for the Galactic warp, of which only 4 involve WN8-9 stars, contrary to previous claims.

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“…The Isaac Newton Telescope Photometric H-alpha Survey of the northern Galactic plane (IPHAS; Drew et al 2005;Barentsen et al 2014), in addition to obtaining filter photometry in the Sloan r and i bands, has produced a large narrow-band Hα photometric sample, enabling many emission line stars and nebulae to be identified and measured. Data from IPHAS have been used to identify new examples of young stellar objects (Vink et al 2008), classical Be stars Raddi et al (2015), supernova remnants (Sabin et al 2013) and planetary nebulae (Mampaso et al 2006;Corradi et al 2011;Viironen et al 2009a;Sabin et al 2014).…”

Section: Introductionmentioning

confidence: 99%

“…From the initial IPHAS data release (González-Solares et al 2008) to the second data release (Barentsen et al 2014) the applications of IPHAS data have expanded. Sale et al (2009), Sale (2012) and Sale et al (2014) have demonstrated how the information from colours using the r , i and (in particular) Hα filters enables spectral types and interstellar dust extinctions to be inferred for objects in the IPHAS survey, enabling 3D extinction mapping to be carried out for sight lines covered by the survey.…”

Section: Introductionmentioning

confidence: 99%

H$α$ fluxes and extinction distances for planetary nebulae in the IPHAS survey of the Northern Galactic Plane

Dharmawardena,

Barlow,

Drew

et al. 2020

Preprint

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We report Hα filter photometry for 197 northern hemisphere planetary nebulae (PNe) obtained using imaging data from the IPHAS survey. Hα+[N ii] fluxes were measured for 46 confirmed or possible PNe discovered by the IPHAS survey and for 151 previously catalogued PNe that fell within the area of the northern Galactic Plane surveyed by IPHAS. After correcting for [N ii] emission admitted by the IPHAS Hα filter, the resulting Hα fluxes were combined with published radio free-free fluxes and Hβ fluxes, in order to estimate mean optical extinctions to 143 PNe using ratios involving their integrated Balmer line fluxes and their extinction-free radio fluxes. Distances to the PNe were then estimated using three different 3D interstellar dust extinction mapping methods, including the IPHAS-based H-MEAD algorithm of Sale (2014). These methods were used to plot dust extinction versus distance relationships for the lines of sight to the PNe; the intercepts with the derived dust optical extinctions allowed distances to the PNe to be inferred. For 17 of the PNe in our sample reliable Gaia DR2 distances were available and these have been compared with the distances derived using three different extinction mapping algorithms as well as with distances from the nebular radius vs. Hα surface brightness relation of Frew et al. (2016). That relation and the H-MEAD extinction mapping algorithm yielded the closest agreement with the Gaia DR2 distances.

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Paul, Founder of Churches

Cited by 16 publications

References 0 publications

Constraints on star formation in NGC 2264

Constraints on star formation in NGC 2264

Unlocking Galactic Wolf-Rayet stars with $\textit{Gaia}$ DR2 I: Distances and absolute magnitudes

H$α$ fluxes and extinction distances for planetary nebulae in the IPHAS survey of the Northern Galactic Plane

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