Gaia-ESO Survey: Gas dynamics in the Carina nebula through optical emission lines

Rosaria Bonito, Klutsch, Costado, Sacco, Bayo, Worley, Lardo, Casey, Damiani, Dorda, Magrini, Koposov, Mapelli, Hourihane, Franciosini, Kalari, Flaccomio, Morbidelli, Gilmore, CarraroPancino, Zwitter, Maíz Apellániz, Lanzafame, Randich, Alfaro, Monaco, Gilmore, Prisinzano, Bonito, Lewis, Zaggia, Micela

Risultato della ricerca: Article

8 Citazioni (Scopus)

Abstract

Aims. We present observations from the Gaia-ESO Survey in the lines of Hα, [N II], [S II], and He I of nebular emission in the central part of the Carina nebula. Methods. We investigate the properties of the two already known kinematic components (approaching and receding), which account for the bulk of emission. Moreover, we investigate the features of the much less known low-intensity high-velocity (absolute RV >50 km s-1) gas emission. Results. We show that gas giving rise to Hα and He I emission is dynamically well correlated with but not identical to gas seen through forbidden-line emission. Gas temperatures are derived from line-width ratios, and densities from [S II] doublet ratios. The spatial variation of N ionization is also studied, and found to differ between the approaching and receding components. The main result is that the bulk of the emission lines in the central part of Carina arise from several distinct shell-like expanding regions, the most evident found around η Car, the Trumpler 14 core, and the star WR25. These "shells" are non-spherical and show distortions probably caused by collisions with other shells or colder, higher-density gas. Some of them are also partially obscured by foreground dust lanes, while very little dust is found in their interior. Preferential directions, parallel to the dark dust lanes, are found in the shell geometries and physical properties, probably related to strong density gradients in the studied region. We also find evidence that the ionizing flux emerging from η Car and the surrounding Homunculus nebula varies with polar angle. The high-velocity components in the wings of Hα are found to arise from expanding dust reflecting the η Car spectrum.
Lingua originaleEnglish
pagine (da-a)A74-
Numero di pagine22
RivistaASTRONOMY & ASTROPHYSICS
Volume591
Stato di pubblicazionePublished - 2016

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gas dynamics
nebulae
European Southern Observatory
light emission
dust
gas
shell
automobile
gases
gas density
gas temperature
wings
emerging
ionization
kinematics
spatial variation
physical property
physical properties
collision
geometry

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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Gaia-ESO Survey: Gas dynamics in the Carina nebula through optical emission lines. / Bonito, Rosaria; Klutsch; Costado; Sacco; Bayo; Worley; Lardo; Casey; Damiani; Dorda; Magrini; Koposov; Mapelli; Hourihane; Franciosini; Kalari; Flaccomio; Morbidelli; Gilmore; Carraro; Pancino; Zwitter; Maíz Apellániz; Lanzafame; Randich; Alfaro; Monaco; Gilmore; Prisinzano; Bonito; Lewis; Zaggia; Micela.

In: ASTRONOMY & ASTROPHYSICS, Vol. 591, 2016, pag. A74-.

Risultato della ricerca: Article

Bonito, R, Klutsch, Costado, Sacco, Bayo, Worley, Lardo, Casey, Damiani, Dorda, Magrini, Koposov, Mapelli, Hourihane, Franciosini, Kalari, Flaccomio, Morbidelli, Gilmore, Carraro, Pancino, Zwitter, Maíz Apellániz, Lanzafame, Randich, Alfaro, Monaco, Gilmore, Prisinzano, Bonito, Lewis, Zaggia & Micela 2016, 'Gaia-ESO Survey: Gas dynamics in the Carina nebula through optical emission lines', ASTRONOMY & ASTROPHYSICS, vol. 591, pagg. A74-.
Bonito, Rosaria ; Klutsch ; Costado ; Sacco ; Bayo ; Worley ; Lardo ; Casey ; Damiani ; Dorda ; Magrini ; Koposov ; Mapelli ; Hourihane ; Franciosini ; Kalari ; Flaccomio ; Morbidelli ; Gilmore ; Carraro ; Pancino ; Zwitter ; Maíz Apellániz ; Lanzafame ; Randich ; Alfaro ; Monaco ; Gilmore ; Prisinzano ; Bonito ; Lewis ; Zaggia ; Micela. / Gaia-ESO Survey: Gas dynamics in the Carina nebula through optical emission lines. In: ASTRONOMY & ASTROPHYSICS. 2016 ; Vol. 591. pagg. A74-.
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title = "Gaia-ESO Survey: Gas dynamics in the Carina nebula through optical emission lines",
abstract = "Aims. We present observations from the Gaia-ESO Survey in the lines of Hα, [N II], [S II], and He I of nebular emission in the central part of the Carina nebula. Methods. We investigate the properties of the two already known kinematic components (approaching and receding), which account for the bulk of emission. Moreover, we investigate the features of the much less known low-intensity high-velocity (absolute RV >50 km s-1) gas emission. Results. We show that gas giving rise to Hα and He I emission is dynamically well correlated with but not identical to gas seen through forbidden-line emission. Gas temperatures are derived from line-width ratios, and densities from [S II] doublet ratios. The spatial variation of N ionization is also studied, and found to differ between the approaching and receding components. The main result is that the bulk of the emission lines in the central part of Carina arise from several distinct shell-like expanding regions, the most evident found around η Car, the Trumpler 14 core, and the star WR25. These {"}shells{"} are non-spherical and show distortions probably caused by collisions with other shells or colder, higher-density gas. Some of them are also partially obscured by foreground dust lanes, while very little dust is found in their interior. Preferential directions, parallel to the dark dust lanes, are found in the shell geometries and physical properties, probably related to strong density gradients in the studied region. We also find evidence that the ionizing flux emerging from η Car and the surrounding Homunculus nebula varies with polar angle. The high-velocity components in the wings of Hα are found to arise from expanding dust reflecting the η Car spectrum.",
keywords = "Astronomy and Astrophysics, HII regions, ISM: general, ISM: individual objects: Carina nebula, Space and Planetary Science",
author = "Rosaria Bonito and Klutsch and Costado and Sacco and Bayo and Worley and Lardo and Casey and Damiani and Dorda and Magrini and Koposov and Mapelli and Hourihane and Franciosini and Kalari and Flaccomio and Morbidelli and Gilmore and Carraro and Pancino and Zwitter and {Ma{\'i}z Apell{\'a}niz} and Lanzafame and Randich and Alfaro and Monaco and Gilmore and Prisinzano and Bonito and Lewis and Zaggia and Micela",
year = "2016",
language = "English",
volume = "591",
pages = "A74--",
journal = "ASTRONOMY & ASTROPHYSICS",
issn = "1432-0746",

}

TY - JOUR

T1 - Gaia-ESO Survey: Gas dynamics in the Carina nebula through optical emission lines

AU - Bonito, Rosaria

AU - Klutsch, null

AU - Costado, null

AU - Sacco, null

AU - Bayo, null

AU - Worley, null

AU - Lardo, null

AU - Casey, null

AU - Damiani, null

AU - Dorda, null

AU - Magrini, null

AU - Koposov, null

AU - Mapelli, null

AU - Hourihane, null

AU - Franciosini, null

AU - Kalari, null

AU - Flaccomio, null

AU - Morbidelli, null

AU - Gilmore, null

AU - Carraro, null

AU - Pancino, null

AU - Zwitter, null

AU - Maíz Apellániz, null

AU - Lanzafame, null

AU - Randich, null

AU - Alfaro, null

AU - Monaco, null

AU - Gilmore, null

AU - Prisinzano, null

AU - Bonito, null

AU - Lewis, null

AU - Zaggia, null

AU - Micela, null

PY - 2016

Y1 - 2016

N2 - Aims. We present observations from the Gaia-ESO Survey in the lines of Hα, [N II], [S II], and He I of nebular emission in the central part of the Carina nebula. Methods. We investigate the properties of the two already known kinematic components (approaching and receding), which account for the bulk of emission. Moreover, we investigate the features of the much less known low-intensity high-velocity (absolute RV >50 km s-1) gas emission. Results. We show that gas giving rise to Hα and He I emission is dynamically well correlated with but not identical to gas seen through forbidden-line emission. Gas temperatures are derived from line-width ratios, and densities from [S II] doublet ratios. The spatial variation of N ionization is also studied, and found to differ between the approaching and receding components. The main result is that the bulk of the emission lines in the central part of Carina arise from several distinct shell-like expanding regions, the most evident found around η Car, the Trumpler 14 core, and the star WR25. These "shells" are non-spherical and show distortions probably caused by collisions with other shells or colder, higher-density gas. Some of them are also partially obscured by foreground dust lanes, while very little dust is found in their interior. Preferential directions, parallel to the dark dust lanes, are found in the shell geometries and physical properties, probably related to strong density gradients in the studied region. We also find evidence that the ionizing flux emerging from η Car and the surrounding Homunculus nebula varies with polar angle. The high-velocity components in the wings of Hα are found to arise from expanding dust reflecting the η Car spectrum.

AB - Aims. We present observations from the Gaia-ESO Survey in the lines of Hα, [N II], [S II], and He I of nebular emission in the central part of the Carina nebula. Methods. We investigate the properties of the two already known kinematic components (approaching and receding), which account for the bulk of emission. Moreover, we investigate the features of the much less known low-intensity high-velocity (absolute RV >50 km s-1) gas emission. Results. We show that gas giving rise to Hα and He I emission is dynamically well correlated with but not identical to gas seen through forbidden-line emission. Gas temperatures are derived from line-width ratios, and densities from [S II] doublet ratios. The spatial variation of N ionization is also studied, and found to differ between the approaching and receding components. The main result is that the bulk of the emission lines in the central part of Carina arise from several distinct shell-like expanding regions, the most evident found around η Car, the Trumpler 14 core, and the star WR25. These "shells" are non-spherical and show distortions probably caused by collisions with other shells or colder, higher-density gas. Some of them are also partially obscured by foreground dust lanes, while very little dust is found in their interior. Preferential directions, parallel to the dark dust lanes, are found in the shell geometries and physical properties, probably related to strong density gradients in the studied region. We also find evidence that the ionizing flux emerging from η Car and the surrounding Homunculus nebula varies with polar angle. The high-velocity components in the wings of Hα are found to arise from expanding dust reflecting the η Car spectrum.

KW - Astronomy and Astrophysics

KW - HII regions

KW - ISM: general

KW - ISM: individual objects: Carina nebula

KW - Space and Planetary Science

UR - http://hdl.handle.net/10447/224103

UR - http://www.edpsciences.org/journal/index.cfm?edpsname=aa

M3 - Article

VL - 591

SP - A74-

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 1432-0746

ER -