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

被引：13

作者：

Damiani, F. ^{[1
]}

Bonito, R. ^{[1
,2
]}

Magrini, L. ^{[3
]}

Prisinzano, L. ^{[1
]}

Mapelli, M. ^{[4
]}

Micela, G. ^{[1
]}

Kalari, V. ^{[5
,6
]}

Maiz Apellaniz, J. ^{[7
]}

Gilmore, G. ^{[8
]}

Randich, S. ^{[3
]}

Alfaro, E. ^{[9
]}

Flaccomio, E. ^{[1
]}

Koposov, S. ^{[8
,10
]}

Klutsch, A. ^{[11
]}

Lanzafame, A. C. ^{[12
]}

Pancino, E. ^{[3
,13
,14
]}

Sacco, G. G. ^{[3
]}

Bayo, A. ^{[15
]}

Carraro, G. ^{[16
]}

Casey, A. R. ^{[8
]}

Costado, M. T. ^{[9
]}

Franciosini, E. ^{[3
]}

Hourihane, A. ^{[8
]}

Lardo, C. ^{[17
]}

Lewis, J. ^{[8
]}

Monaco, L. ^{[18
]}

Morbidelli, L. ^{[3
]}

Worley, C. ^{[8
]}

Zaggia, S. ^{[19
]}

Zwitter, T. ^{[20
]}

Dorda, R. ^{[21
]}

机构：

[1] INAF Osservatorio Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy

[2] Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy

[3] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy

[4] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[5] Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland

[6] Queens Univ Belfast, Sch Math & Phys, Belfast BT61 7NN, Antrim, North Ireland

[7] Ctr Astrobiol CSIC INTA, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain

[8] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[9] CSIC, Inst Astrofis Andalucia, Apdo 3004, Granada 18080, Spain

[10] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia

[11] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy

[12] Univ Catania, Dipartimento Fis & Astron, Sez Astrofis, Via S Sofia 78, I-95123 Catania, Italy

[13] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy

[14] ASI Sci Data Ctr, Via Politecn SNC, I-00133 Rome, Italy

[15] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile

[16] European Southern Observ, Alonso Cordova 3107 Vitacura, Santiago, Chile

[17] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[18] Univ Andres Bello, Dept Ciencias Fis, Republ 220, Santiago, Chile

[19] INAF Padova Observ, Vicolo Osservatorio 5, I-35122 Padua, Italy

[20] Univ Ljubljana, Fac Math & Phys, Jadranska 19, Ljubljana 1000, Slovenia

[21] Univ Alicante, Dept Fis Ingn Sistemas & Teoria Senal, Apdo 99, E-03080 Alicante, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2016年 / 591卷

基金：

英国科学技术设施理事会;

关键词：

ISM: individual objects: Carina nebula; ISM: general; HII regions; ETA-CARINAE; TRUMPLER; 16; COMPLEX; CHANDRA; HOMUNCULUS; SHAPE;

D O I：

10.1051/0004-6361/201628169

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. We present observations from the Gaia-ESO Survey in the lines of H alpha, [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 H alpha 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 eta 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 eta Car and the surrounding Homunculus nebula varies with polar angle. The high-velocity components in the wings of H alpha are found to arise from expanding dust reflecting the eta Car spectrum.

引用

页数：22

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