eprintid: 10095260
rev_number: 14
eprint_status: archive
userid: 608
dir: disk0/10/09/52/60
datestamp: 2020-05-13 12:05:32
lastmod: 2021-10-05 00:18:16
status_changed: 2020-05-13 12:05:32
type: article
metadata_visibility: show
creators_name: James, BL
creators_name: Tsamis, YG
creators_name: Walsh, JR
creators_name: Barlow, MJ
creators_name: Westmoquette, MS
title: The Lyman break analogue Haro 11: spatially resolved chemodynamics with VLT FLAMES
ispublished: pub
divisions: UCL
divisions: B04
divisions: C06
divisions: F60
keywords: stars: Wolf–Rayet, galaxies: abundances, galaxies: dwarf, galaxies: individual: Haro 11, galaxies: interactions, galaxies: kinematics and dynamics
note: This version is the version of record. For information on re-use, please refer to the publisher’s terms and conditions.
abstract: Using VLT/Fibre Large Array Multi Element Spectrograph (FLAMES) optical integral field unit observations, we present the first spatially resolved spectroscopic study of the well-known blue compact galaxy Haro 11, thought to be a local analogue to high-redshift Lyman break galaxies. Haro 11 displays complex emission line profiles, consisting of narrow (full width at half-maximum, FWHM ≲ 200 km s−1) and broad (FWHM ∼ 200–300 km s−1) components. We identify three distinct emission knots kinematically connected to one another. A chemodynamical analysis is presented, revealing that spatially resolved ionic and elemental abundances do not agree with those derived from integrated spectra across the galaxy. We conclude that this is almost certainly due to the surface brightness weighting of electron temperature in integrated spectra, leading to higher derived abundances. We find that the eastern knot has a low gas density, but a higher temperature (by ∼4000 K) and consequently an oxygen abundance ∼0.4 dex lower than the neighbouring regions. A region of enhanced N/O is found specifically in Knot C, confirming previous studies that found anomalously high N/O ratios in this system. Maps of the Wolf–Rayet (WR) feature at 4686 Å reveal large WR populations (∼900–1500 stars) in Knots A and B. The lack of WR stars in Knot C combined with an age of ∼7.4 Myr suggests that a recently completed WR phase may be responsible for the observed N/O excess. Conversely, the absence of N-enriched gas and strong WR emission in Knots A and B suggests that we are observing these regions at an epoch where stellar ejecta has yet to cool and mix with the interstellar medium.
date: 2013-04-11
date_type: published
publisher: OXFORD UNIV PRESS
official_url: https://doi.org/10.1093/mnras/stt034
oa_status: green
full_text_type: pub
language: eng
primo: open
primo_central: open_green
verified: verified_manual
elements_id: 844411
doi: 10.1093/mnras/stt034
lyricists_name: Barlow, Michael
lyricists_id: MJBAR75
actors_name: Barlow, Michael
actors_id: MJBAR75
actors_role: owner
full_text_status: public
publication: Monthly Notices of the Royal Astronomical Society
volume: 430
number: 3
pagerange: 2097-2112
pages: 16
citation:        James, BL;    Tsamis, YG;    Walsh, JR;    Barlow, MJ;    Westmoquette, MS;      (2013)    The Lyman break analogue Haro 11: spatially resolved chemodynamics with VLT FLAMES.                   Monthly Notices of the Royal Astronomical Society , 430  (3)   pp. 2097-2112.    10.1093/mnras/stt034 <https://doi.org/10.1093/mnras%2Fstt034>.       Green open access   
 
document_url: https://discovery.ucl.ac.uk/id/eprint/10095260/1/james13_haro11.pdf