2017A&A...608A...7F


Query : 2017A&A...608A...7F

2017A&A...608A...7F - Astronomy and Astrophysics, volume 608A, 7-7 (2017/12-1)

The MUSE Hubble Ultra Deep Field Survey. VII. Fe II* emission in star-forming galaxies.

FINLEY H., BOUCHE N., CONTINI T., PAALVAST M., BOOGAARD L., MASEDA M., BACON R., BLAIZOT J., BRINCHMANN J., EPINAT B., FELTRE A., MARINO R.A., MUZAHID S., RICHARD J., SCHAYE J., VERHAMME A., WEILBACHER P.M. and WISOTZKI L.

Abstract (from CDS):

Non-resonant FeII* (λ2365, λ2396, λ2612, λ2626) emission can potentially trace galactic winds in emission and provide useful constraints to wind models. From the 3.15'x3.15' mosaic of the Hubble Ultra Deep Field (UDF) obtained with the VLT/MUSE integral field spectrograph, we identify a statistical sample of 40 FeII* emitters and 50 MgII (λλ2796,2803) emitters from a sample of 271 [OII]λλ3726,3729 emitters with reliable redshifts from z=0.85-1.50 down to 2x10–18 (3σ)ergs/s/cm2 (for [OII]), covering the M* range from 108-1011M. The FeII* and MgII emitters follow the galaxy main sequence, but with a clear dichotomy. Galaxies with masses below 109M and star formation rates (SFRs) of ≤1M/yr have MgII emission without accompanying FeII* emission, whereas galaxies with masses above 1010M and SFRs≥10M/yr have FeII* emission without accompanying MgII emission. Between these two regimes, galaxies have both MgII and FeII* emission, typically with MgII P Cygni profiles. Indeed, the MgII profile shows a progression along the main sequence from pure emission to P Cygni profiles to strong absorption, due to resonant trapping. Combining the deep MUSE data with HST ancillary information, we find that galaxies with pure MgII emission profiles have lower SFR surface densities than those with either MgII P Cygni profiles or FeII* emission. These spectral signatures produced through continuum scattering and fluorescence, MgII P Cygni profiles and FeII* emission, are better candidates for tracing galactic outflows than pure MgII emission, which may originate from HII regions. We compare the absorption and emission rest-frame equivalent widths for pairs of FeII transitions to predictions from outflow models and find that the observations consistently have less total re-emission than absorption, suggesting either dust extinction or non-isotropic outflow geometries.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: evolution - galaxies: ISM - ISM: jets and outflows - ultraviolet: ISM - ultraviolet: ISM

Simbad objects: 17

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Number of rows : 17
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 [LBX2017] 689 AGN 03 32 36.436 -27 46 31.52 24.1001 23.7705 23.36 23.04 22.93 ~ 22 0
2 GOODS J033236.56-274640.6 G 03 32 36.560 -27 46 40.61 25.2760 25.1319 25.070   25.0235 ~ 17 0
3 GOODS-MUSIC 10921 G 03 32 36.590 -27 46 39.72 26.1311 26.0551 26.14     ~ 10 0
4 CXOCDFS J033236.6-274631 AGN 03 32 36.666 -27 46 31.04 25.4931 22.1392 24.029 23.57 22.609 ~ 49 0
5 GOODS J033237.73-274642.7 G 03 32 37.729 -27 46 42.68 24.8646 24.6520 24.602   24.4677 ~ 21 0
6 EIS-DEEP CDFS-2 Ks 1 1516 G 03 32 38.098 -27 46 13.91 24.0450 23.9119 23.536 23.51   ~ 23 0
7 [IBB2017] 36 G 03 32 38.245 -27 46 30.10 26.0119 25.6353 25.17   24.7157 ~ 20 0
8 UDF 7081 G 03 32 38.968 -27 46 56.31 25.0156 24.6517 24.97     ~ 13 0
9 NAME Hubble Ultra Deep Field reg 03 32 39.0 -27 47 29           ~ 1463 0
10 GOODS-MUSIC 10981 EmG 03 32 39.220 -27 46 36.08 25.6247 25.6091 25.62     ~ 11 0
11 [IBB2017] 30 EmG 03 32 39.383 -27 47 14.27 25.0240 24.9342 24.764     ~ 18 0
12 GOODS-MUSIC 10838 EmG 03 32 39.575 -27 46 43.43   25.2445 25.32     ~ 14 0
13 ASPECS LP.3mm.11 G 03 32 39.813 -27 46 53.54 25.0390 24.5628 24.079     ~ 27 0
14 ASPECS LP.3mm.06 QSO 03 32 39.883 -27 47 15.06 23.3163 23.0619 22.604 22.41 21.765 ~ 49 0
15 NAME Fermi Bubbles bub 17 45 -29.0           ~ 344 0
16 [LFR2003] 314 G 22 32 52.1962 -60 33 23.784 24.762 23.858 23.514   22.83 ~ 14 0
17 NAME HDF-S reg 22 32 56 -60 33.0           ~ 553 0

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2022.05.24-10:05:51

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