J/ApJ/814/L6 CIII] emission in near & far star-forming galaxies (Rigby+, 2015)
C III] emission in star-forming galaxies near and far.
Rigby J.R., Bayliss M.B., Gladders M.D., Sharon K., Wuyts E., Dahle H.,
Johnson T., Pena-Guerrero M.
<Astrophys. J., 814, L6 (2015)>
=2015ApJ...814L...6R 2015ApJ...814L...6R (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Equivalent widths ; Gravitational lensing
Keywords: galaxies: star formation; gravitational lensing: strong;
techniques: spectroscopic
Abstract:
We measure [C III] 1907, C III] 1909Å emission lines in 11
gravitationally lensed star-forming galaxies at z∼1.6-3, finding much
lower equivalent widths than previously reported for fainter lensed
galaxies. While it is not yet clear what causes some galaxies to be
strong C III] emitters, C III] emission is not a universal property of
distant star-forming galaxies. We also examine C III] emission in 46
star-forming galaxies in the local universe, using archival spectra
from GHRS, FOS, and STIS on HST and IUE. Twenty percent of these local
galaxies show strong C III] emission, with equivalent widths ←5Å.
Three nearby galaxies show C III] emission equivalent widths as large
as the most extreme emitters yet observed in the distant universe; all
three are Wolf-Rayet galaxies. At all redshifts, strong C III]
emission may pick out low-metallicity galaxies experiencing intense
bursts of star formation. Such local C iii] emitters may shed light on
the conditions of star formation in certain extreme high-redshift
galaxies.
Description:
We measure the equivalent widths of Lyα and the C III] doublet
in the rest-frame UV spectra of 11 gravitationally lensed galaxies at
1.6<z<3.1. Spectra were obtained using the MagE spectrograph on the
Clay Magellan II telescope, as part of a large study of the rest-frame
ultraviolet spectral properties of bright lensed galaxies (J. R. Rigby
et al. 2016, in preparation). We also take C III] equivalent widths
from literature (see section 2).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 118 71 Galaxy samples, properties, and equivalent widths
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See also:
II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009)
J/A+A/529/A149 : HII regions in low-metallicity galaxies (Guseva+, 2011)
J/ApJS/164/81 : Spectrophotometry of nearby galaxies (Moustakas+, 2006)
J/A+AS/136/35 : WR galaxies and HII regions catalog (Schaerer+ 1999)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 25 A25 --- Name Galaxy/Object name
26- 34 F9.6 --- z [-0.0008/3.1] Redshift
36- 36 I1 --- r_z ? Reference for redshift (1)
38 A1 --- l_[O/H] Limit flag on Metallicity, [O/H]
39- 42 F4.2 --- [O/H] [0/9.2]? Metallicity, 12+log[O/H]
45- 48 F4.2 --- E_[O/H] [0.02/0.1]? Uncertainty on [O/H], upper bound
51- 54 F4.2 --- e_[O/H] [0.02/0.2]? Uncertainty on [O/H], lower bound
56- 59 A4 --- r_[O/H] Indicates source of measurement for
metallicity (2)
61- 61 A1 --- l_WrLya Upper or Lower limit flag on WrLya
62- 67 F6.2 0.1nm WrLya [-82.6/8.2]? Rest-frame equivalent width
of Lyman alpha (3)
69- 74 F6.2 0.1nm e_WrLya [0.1/29.2]? Uncertainty on WrLya
76- 79 A4 --- r_WrLya Indicates source of measurement for WrLya (2)
81- 81 A1 --- l_WCIII Upper or Lower limit flag on WCIII
82- 88 F7.3 0.1nm WCIII [-27/0.8]? Rest-frame equivalent width of
C [III] 1907,1909 doublet (4)
90- 96 F7.3 0.1nm e_WCIII [0.009/13]? Uncertainty on WCIII
98-101 A4 --- r_WCIII Indicates source of measurement for WCIII (2)
103-106 A4 --- Set Which sample this galaxy belongs to (2)
108-108 A1 --- Filt [Rg] Filter for galaxy/object, AB magnitude
110-114 F5.2 mag mag [19.1/21.8]? Galaxy/object AB magnitude in Filt
(MagEmag)
116-118 A3 --- r_mag Reference for mag (2)
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Note (1): Source of redshifts as follows:
0 = Redshifts for z∼0 galaxies are from NED
1 = Rigby et al. (2014ApJ...790...44R 2014ApJ...790...44R) and Rigby et al., in prep.
2 = Bordoloi et al. 2015 (submitted; arXiv:1602.07700)
Note (2): Reference codes as follows:
A09 = Abazajian et al. 2009 (II/294)
B07 = Belokurov et al. (2007ApJ...671L...9B 2007ApJ...671L...9B)
B10 = Bian et al. (2010ApJ...725.1877B 2010ApJ...725.1877B)
G96 = Giavalisco et al. (1996ApJ...466..831G 1996ApJ...466..831G)
H09 = Hainline et al. (2009ApJ...701...52H 2009ApJ...701...52H)
K10 = Koester et al. (2010ApJ...723L..73K 2010ApJ...723L..73K)
L11 = Leitherer et al. (2011AJ....141...37L 2011AJ....141...37L)
PG15 = Pena-Guerrero et al. (in prep.)
R14 = Rigby et al. (2014ApJ...790...44R 2014ApJ...790...44R)
S07 = Smail et al. (2007ApJ...654L..33S 2007ApJ...654L..33S)
W10 = Wuyts et al. (2010ApJ...724.1182W 2010ApJ...724.1182W)
W12 = Wuyts et al. (2012ApJ...755...73W 2012ApJ...755...73W)
W14 = Wuyts et al. (2014ApJ...781...61W 2014ApJ...781...61W)
Telescope/Instrument codes as follows:
MagE = Clay Magellan II telescope, MagE spectrograph spectra
FIRE = Baade Magellan telescope, FIRE spectrometer spectra
IUE = Archival International Ultraviolet Explorer (IUE) spectra
STIS = HST/STIS spectra
FOS = HST/FOS spectra
Note (3): Rest-frame equivalent width of Lyman alpha, in units of Angstroms.
Emission is negative, absorption is positive.
Note (4): Rest-frame equivalent width of C III] 1907,1909 doublet, in units of
Angstroms. When doublet is resolved, this is the sum of both transitions.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 04-Mar-2016