FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W3048136912> ?p ?o ?g. }

• W3048136912 endingPage "A56" @default.
• W3048136912 startingPage "A56" @default.
• W3048136912 abstract "Context. NGC 2264 is a young cluster whose accretion properties can be investigated in detail by taking advantage of the FLAMES data in the context of the Gaia -ESO Survey. In fact, the analysis of the H α emission line profile can provide us with information about the accretion and ejection activity of young stars. However, a strong nebular emission that contributes to the H α emission can alter the profiles, with consequences for their physical interpretation. Aims. Our study is aimed at investigating the accretion and ejection properties of NGC 2264 by applying a proper treatment of the sky contribution to the H α and forbidden emission lines (FELs; [SII] and [NII] doublets). Methods. We developed a tool, the OH α NA-method, to handle the strong nebular contribution and spectra with spurious profiles of the H α and FELs, namely altered H α profiles or absorption features artificially created where emission lines (FELs) are expected. We derived the quantitative measurements of relevant parameters to describe the accretion and ejection processes in young members of NGC 2264, focusing on reliable quantities derived from the width of the lines, which is relatively unaffected by the nebular emission, unlike the intensity peak, which can be altered significantly. Results. We derive the quantitative measurements related to the H α emission line and discuss the comparison between the original and sky-subtracted spectra. We thus reveal possible profile alterations with consequences for their physical interpretation. Furthermore, we show the analysis of the variability for multi-epoch observations, also deriving the velocity of the infalling and outflowing plasma from the wings of the broad H α emission line (in accreting stars). We also explore the mass accretion rate versus full width at zero intensity of the H α line, namely Ṁ versus FWZI(H α ), a correlation based on the width of the emission line, which is expected to be more robust with respect to any measurement derived from the peak (e.g., H α 10% ) and possibly altered by the nebular contribution. Conclusions. We are able to ascertain that more than 20% of the confirmed accretors, which have already been identified in NGC 2264, are affected by the alteration of their line profiles due to the contribution of the nebular emission. Therefore, this is an important issue to consider when investigating accretion and ejection processes in young stellar clusters. While a small fraction of spectra can be unequivocally classified as either unaffected by nebular emission or dominated by nebular emission, the majority (> 90%) represent intermediate cases whose spectral features have to be investigated in detail to derive reliable measurements of the relevant parameters and their physical implications." @default.
• W3048136912 created "2020-08-13" @default.
• W3048136912 creator A5000983008 @default.
• W3048136912 creator A5004591084 @default.
• W3048136912 creator A5005853340 @default.
• W3048136912 creator A5008041848 @default.
• W3048136912 creator A5008522421 @default.
• W3048136912 creator A5013616764 @default.
• W3048136912 creator A5014987275 @default.
• W3048136912 creator A5023878393 @default.
• W3048136912 creator A5024489492 @default.
• W3048136912 creator A5024946777 @default.
• W3048136912 creator A5025394421 @default.
• W3048136912 creator A5031945322 @default.
• W3048136912 creator A5033947343 @default.
• W3048136912 creator A5035049404 @default.
• W3048136912 creator A5035800367 @default.
• W3048136912 creator A5039986610 @default.
• W3048136912 creator A5044292055 @default.
• W3048136912 creator A5045792808 @default.
• W3048136912 creator A5052374418 @default.
• W3048136912 creator A5052845622 @default.
• W3048136912 creator A5057789592 @default.
• W3048136912 creator A5059639018 @default.
• W3048136912 creator A5078152340 @default.
• W3048136912 creator A5082180004 @default.
• W3048136912 creator A5086323221 @default.
• W3048136912 creator A5087376175 @default.
• W3048136912 creator A5089972304 @default.
• W3048136912 creator A5090171569 @default.
• W3048136912 creator A5090439959 @default.
• W3048136912 creator A5091275930 @default.
• W3048136912 date "2020-10-01" @default.
• W3048136912 modified "2023-10-13" @default.
• W3048136912 title "The <i>Gaia</i>-ESO Survey: A new diagnostic for accretion and outflow activity in the young cluster NGC 2264" @default.
• W3048136912 cites W1973213041 @default.
• W3048136912 cites W1978391636 @default.
• W3048136912 cites W1984303403 @default.
• W3048136912 cites W1998757246 @default.
• W3048136912 cites W2045672790 @default.
• W3048136912 cites W2057156016 @default.
• W3048136912 cites W2065500942 @default.
• W3048136912 cites W2078216201 @default.
• W3048136912 cites W2105482436 @default.
• W3048136912 cites W2114822581 @default.
• W3048136912 cites W2136168988 @default.
• W3048136912 cites W2154370253 @default.
• W3048136912 cites W2255950206 @default.
• W3048136912 cites W2344241632 @default.
• W3048136912 cites W2743809863 @default.
• W3048136912 cites W2756296597 @default.
• W3048136912 cites W2950618108 @default.
• W3048136912 cites W2969568124 @default.
• W3048136912 cites W3098422742 @default.
• W3048136912 cites W3098990682 @default.
• W3048136912 cites W3099807012 @default.
• W3048136912 cites W3101303225 @default.
• W3048136912 cites W3101689712 @default.
• W3048136912 cites W3103665099 @default.
• W3048136912 cites W3104386877 @default.
• W3048136912 cites W3121431628 @default.
• W3048136912 cites W4289883362 @default.
• W3048136912 doi "https://doi.org/10.1051/0004-6361/202037942" @default.
• W3048136912 hasPublicationYear "2020" @default.
• W3048136912 type Work @default.
• W3048136912 sameAs 3048136912 @default.
• W3048136912 citedByCount "11" @default.
• W3048136912 countsByYear W30481369122020 @default.
• W3048136912 countsByYear W30481369122021 @default.
• W3048136912 countsByYear W30481369122022 @default.
• W3048136912 countsByYear W30481369122023 @default.
• W3048136912 crossrefType "journal-article" @default.
• W3048136912 hasAuthorship W3048136912A5000983008 @default.
• W3048136912 hasAuthorship W3048136912A5004591084 @default.
• W3048136912 hasAuthorship W3048136912A5005853340 @default.
• W3048136912 hasAuthorship W3048136912A5008041848 @default.
• W3048136912 hasAuthorship W3048136912A5008522421 @default.
• W3048136912 hasAuthorship W3048136912A5013616764 @default.
• W3048136912 hasAuthorship W3048136912A5014987275 @default.
• W3048136912 hasAuthorship W3048136912A5023878393 @default.
• W3048136912 hasAuthorship W3048136912A5024489492 @default.
• W3048136912 hasAuthorship W3048136912A5024946777 @default.
• W3048136912 hasAuthorship W3048136912A5025394421 @default.
• W3048136912 hasAuthorship W3048136912A5031945322 @default.
• W3048136912 hasAuthorship W3048136912A5033947343 @default.
• W3048136912 hasAuthorship W3048136912A5035049404 @default.
• W3048136912 hasAuthorship W3048136912A5035800367 @default.
• W3048136912 hasAuthorship W3048136912A5039986610 @default.
• W3048136912 hasAuthorship W3048136912A5044292055 @default.
• W3048136912 hasAuthorship W3048136912A5045792808 @default.
• W3048136912 hasAuthorship W3048136912A5052374418 @default.
• W3048136912 hasAuthorship W3048136912A5052845622 @default.
• W3048136912 hasAuthorship W3048136912A5057789592 @default.
• W3048136912 hasAuthorship W3048136912A5059639018 @default.
• W3048136912 hasAuthorship W3048136912A5078152340 @default.
• W3048136912 hasAuthorship W3048136912A5082180004 @default.
• W3048136912 hasAuthorship W3048136912A5086323221 @default.
• W3048136912 hasAuthorship W3048136912A5087376175 @default.

• next