C Iii] Emission in Star-Forming Galaxies Near and Far

Rigby, J. Keith; Bayliss, M.; Gladders, Michael D.; Sharon, Keren; Wuyts, Eva; Dahle, H.; Johnson, Traci L.; Peña-Guerrero, María

doi:10.1088/2041-8205/814/1/l6

Cited by 87 publications

(173 citation statements)

References 44 publications

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“…Based on the correlation in strength between C iii] and Mg ii emission (Section 4.3), this result suggests indirectly that stronger C iii] may be found within lower-metallicity galaxies in our sample. Our inferred correlation between C iii] and metallicity is not only consistent with both models and observations of C iii] at other redshifts Rigby et al 2015;Jaskot & Ravindranath 2016), but is also supported by the result that CIII] emission is significantly stronger in the lower-mass half of our sample, given the well-measured correlation between metallicity and stellar mass (e.g., Tremonti et al 2004;Zahid et al 2013). …”

Section: Iii] Vs Metallicitiessupporting

confidence: 89%

“…Photoionization models and observations at different redshifts have revealed that low gas metallicity leads to enhanced nebular C iii] emission due to the hard ionizing SED of the associated metal-poor stars exciting the gas, and the elevated electron temperature resulting from reduced metal cooling (e.g., Erb et al 2010;Stark et al 2014;Rigby et al 2015;Jaskot & Ravindranath 2016, see Section 5.2.2 for a detailed discussion). In order to examine if the correspondence between C iii] emission and metallicity found in high-redshift studies also holds for z ∼ 1, we estimated metallicities using optical emission features.…”

Section: Iii] Vs Metallicitiesmentioning

confidence: 99%

“…Nebular C iii] emission has been studied both in the local universe Leitherer et al 2011;Berg et al 2016, Pena-Guerrero et al 2015 and at redshift > 2 (Shapley et al 2003;Erb et al Furthermore, results from photoionization models indicate that C iii] emission is enhanced at lower gas-phase metallicity, higher ionization parameters and harder radiation fields (e.g., Erb et al 2010;Stark et al 2015Stark et al , 2017Berg et al 2016;Jaskot & Ravindranath 2016). Many studies have also shown that the strength of C iii] correlates with that of other emission features, such as Lyα (Shapley et al 2003;Stark et al 2014Stark et al , 2015Rigby et al 2015;Jaskot & Ravindranath 2016) and [O iii]λ5007 (Jaskot & Ravindranath 2016), in the sense that large C iii] EW tends to appear in galaxies with strong Lyα and [O iii] emission. In principle, strong C iii] emitters at z > 6 are ideal sources to study how C iii] emission relates in general to the properties of host galaxies and other emission lines.…”

Section: Introductionmentioning

confidence: 99%

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C iii] Emission in Star-forming Galaxies at z ∼ 1

Shapley

Martin

et al. 2017

ApJ

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The C iii]λλ1907, 1909 rest-frame UV emission doublet has recently been detected in galaxies during the epoch of reionization (z > 6), with high equivalent width (> 10Å, rest frame). Currently, it is possible to obtain much more detailed information for star-forming galaxies at significantly lower redshift. Accordingly, studies of their far-UV spectra are useful for understanding the factors modulating the strength of C iii] emission. We present the first statistical sample of C iii] emission measurements in star-forming galaxies at z ∼ 1. Our sample is drawn from the DEEP2 survey and spans the redshift 0.64 z 1.35 ( z =1.08). We find that the median equivalent width (EW) of individual C iii] detections in our sample (1.30Å) is much smaller than the typical value observed thus far at z > 6. Furthermore, out of 184 galaxies with coverage of C iii], only 40 have significant detections. Galaxies with individual C iii] detections have bluer colors and lower luminosities on average than those without, implying that strong C iii] emitters are in general young and low-mass galaxies without significant dust extinction. Using stacked spectra, we further investigate how C iii] strength correlates with multiple galaxy properties (M B , U −B, M * , star-formation rate, specific star-formation rate) and rest-frame near-UV (Fe ii* and Mg ii) and optical ([O iii] and Hβ) emission line strengths. These results provide a detailed picture of the physical environment in star-forming galaxies at z ∼ 1, and motivate future observations of strong C iii] emitters at similar redshifts.

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Section: Iii] Vs Metallicitiessupporting

confidence: 89%

Section: Iii] Vs Metallicitiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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C iii] Emission in Star-forming Galaxies at z ∼ 1

Shapley

Martin

et al. 2017

ApJ

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“…Si II) absorption lines from neutral outflowing gas and high-ionization features such as a strong P Cygni stellar wind profile of C IV, which is indicative of stellar winds from very young and massive stars. The observed C III] λλ1907, 1909 Å emission, W r (C III]) = −6 ± 4 Å, is also indicative of an intense burst of star formation that is coupled with low metallicity (Bayliss et al 2014;Rigby et al 2015).…”

Section: Spectroscopymentioning

confidence: 89%

Discovery of an exceptionally bright giant arc atz= 2.369, gravitationally lensed by thePlanckcluster PSZ1 G311.65−18.48

Dahle

Aghanim

Guennou

et al. 2016

A&A

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As part of an all-sky follow-up of the Planck catalogue of Sunyaev-Zeldovich (SZ) cluster candidates detected in the first 14 months of data, we are observing cluster candidates in the southern sky in the optical imaging and spectroscopy through an ESO Large Programme. Inspection of ESO New Technology Telescope (NTT) R-and z-band imaging data from our programme has revealed an unusually large and bright arc in the field of PSZ1 G311.65−18.48. We establish the basic photometric and morphological properties of the arc and provide conclusive evidence for the gravitational lensing nature of this object. Guided by the NTT images, we have obtained a long-slit spectrum with IMACS on the Magellan-I Baade Telescope, covering a part of the arc and the brightest cluster galaxy of PSZ1 G311.65−18.48. Our imaging data confirm the presence of a galaxy cluster coinciding (within 0 .6) with the position of the Planck SZ source. The arc is separated by ∼30 from the brightest cluster galaxy, which closely coincides with the center of curvature of the arc. A photometric analysis yields integrated (Vega) magnitudes of (R, z, J, K s ) = (17. 82, 17.38, 16.75, 15.43) for the arc, more than one magnitude brighter than any previously known lensed arc at z ∼ 2-3. The arc is a vigorously star-forming galaxy at z = 2.369, while the Planck SZ cluster lens is at z = 0.443. Even when allowing for lensing magnifications as high as µ = 100 still leads to the conclusion that the source galaxy is among the intrinsically most luminous normal (i.e., non-AGN) galaxies known at z ∼ 2-3.

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“…The C iii] equivalent width of 7.1Å is very similar to the value of 7.7Å that we measure for the FOS spectrum near cluster #5. Rigby et al (2015) discuss measurements of C iii] emission in nearby and high redshift galaxies. In their nearby sample, they include the FOS spectrum of NGC 5253 used here, and note that this galaxy is one of the 20% of local galaxies that show strong C iii] emission.…”

Section: Comparison With He Ii-emitting High Redshiftmentioning

confidence: 97%

The very massive star content of the nuclear star clusters in NGC 5253

2016

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The blue compact dwarf galaxy NGC 5253 hosts a very young starburst containing twin nuclear star clusters, separated by a projected distance of 5 pc. One cluster (#5) coincides with the peak of the Hα emission and the other (#11) with a massive ultracompact H ii region. A recent analysis of these clusters shows that they have a photometric age of 1 ± 1 Myr, in apparent contradiction with the age of 3-5 Myr inferred from the presence of Wolf-Rayet features in the cluster #5 spectrum. We examine Hubble Space Telescope ultraviolet and Very Large Telescope optical spectroscopy of #5 and show that the stellar features arise from very massive stars (VMS), with masses greater than 100 M , at an age of 1-2 Myr. We further show that the very high ionizing flux from the nuclear clusters can only be explained if VMS are present. We investigate the origin of the observed nitrogen enrichment in the circum-cluster ionized gas and find that the excess N can be produced by massive rotating stars within the first 1 Myr. We find similarities between the NGC 5253 cluster spectrum and those of metal poor, high redshift galaxies. We discuss the presence of VMS in young, star-forming galaxies at high redshift; these should be detected in rest frame UV spectra to be obtained with the James Webb Space Telescope. We emphasize that population synthesis models with upper mass cut-offs greater than 100 M are crucial for future studies of young massive star clusters at all redshifts.

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C Iii] Emission in Star-Forming Galaxies Near and Far

Cited by 87 publications

References 44 publications

C iii] Emission in Star-forming Galaxies at z ∼ 1

C iii] Emission in Star-forming Galaxies at z ∼ 1

Discovery of an exceptionally bright giant arc atz= 2.369, gravitationally lensed by thePlanckcluster PSZ1 G311.65−18.48

The very massive star content of the nuclear star clusters in NGC 5253

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