Galaxy Zoo Green Peas: discovery of a class of compact extremely star-forming galaxies

Cardamone, Carolin N.; Schawinski, Kevin; Sarzi, Marc; Bamford, Steven P.; Bennert, Nicola; Urry, C. Megan; Lintott, Chris; Keel, William C.; Parejko, John K.; Nichol, R. C.; Thomas, Daniel; Andreescu, Dan; Murray, Phil; Raddick, M. Jordan; Slosar, Anže; Szalay, Alexander S.; Vandenberg, Jan

doi:10.1111/j.1365-2966.2009.15383.x

Cited by 581 publications

(818 citation statements)

References 107 publications

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“…Although there appear to be no low redshift analogues of GDS18.92−02.7, the recent discovery of "Green Peas" by the Galaxy Zoo project (Cardamone et al 2009) does, however, show that there exists a population of compact, strong…”

Section: Discussionmentioning

confidence: 99%

Ly$\mathsf{\alpha}$ emitters in the GOODS-S field

Raiter¹,

Fosbury

Teimoorinia

2010

A&A

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Context. The Great Observatories Origins Deep Survey (GOODS) has provided us with one of the deepest multi-wavelength views of the distant universe. The combination of multi-band photometry and optical spectroscopy has resulted in the identification of sources whose redshifts extend to values in excess of six. Amongst these distant sources are Lyα emitters whose nature must be deduced by clearly identifying the different components that contribute to the measured SED. Aims. From a sample of Lyα emitters in the GOODS-S field with uncontaminated photometry and optical (red) spectroscopy, we select a spatially compact object at a redshift of 5.563 (Lyα) that shows a second emission line, identified as N iv] 1486 Å. The SED is modelled in a way that accounts for both the N iv] line emission and the photometry in a self-consistent way.Methods. The photoionization code CLOUDY is used to calculate a range of nebular models as a function of stellar ionizing source temperature, ionization parameter, density and nebular metallicity. We compare the theoretical and observed magnitudes and search for the model parameters that also reproduce the observed N iv] luminosity and equivalent width.Results. A nebular model with a hot blackbody ionizing source of around 100 kK and a nebular metallicity of ∼5% of solar is able to fit the observed SED and, in particular, explain the large apparent Balmer break which is inferred from the pure stellar population model fitting conventionally applied to multi-band photometric observations. In our model, an apparent spectral break is produced by strong [O iii] 4959, 5007 Å emission falling in one of the IR bands (IRAC1 in this case). A lower limit on the total baryonic mass of a model of this type is 3.2 × 10 8 M . Conclusions. It is argued that objects with Lyα emission at high redshift that show an apparent Balmer break may have their SED dominated by nebular emission and so could possibly be identified with very young starbursting galaxies rather than massive evolved stellar populations. Detailed studies of these emission nebulae with large telescopes will provide a unique insight into very early chemical evolution.

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Section: Discussionmentioning

confidence: 99%

Ly$\mathsf{\alpha}$ emitters in the GOODS-S field

Raiter¹,

Fosbury

Teimoorinia

2010

A&A

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“…The tadpoles have high Hα velocity dispersion and show evidence for marginal rotation dominance (Sánchez Almeida et al 2013). Yet another class of rare lowmass galaxies which might be similar to high-redshift objects are the 'green peas' 15 first discovered by public volunteers inspecting SDSS images in the Galaxy Zoo project (Cardamone et al 2009). These are very compact (2-3 kpc) low mass (10 8 -10 10 M ࣻ ) but with high star-formation rates (>10-30 M ࣻ yr −1 ), low metallicities and have complex kinematics with velocity dispersions of 30-80 km s −1 (Amorín et al 2012) suggesting similarities (apart from the substantially lower stellar masses) to the 'dispersion-dominated' objects seen at high-redshift (see Section 5.2).…”

Section: 'Local Analogue' Samplesmentioning

confidence: 99%

The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time

Glazebrook

2013

Publ. Astron. Soc. Aust.

136

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The last seven years have seen an explosion in the number of Integral Field galaxy surveys, obtaining resolved 2D spectroscopy, especially at high-redshift. These have taken advantage of the mature capabilities of 8-10 m class telescopes and the development of associated technology such as AO. Surveys have leveraged both high spectroscopic resolution enabling internal velocity measurements and high spatial resolution from AO techniques and sites with excellent natural seeing. For the first time, we have been able to glimpse the kinematic state of matter in young, assembling starforming galaxies and learn detailed astrophysical information about the physical processes and compare their kinematic scaling relations with those in the local Universe. Observers have measured disc galaxy rotation, merger signatures, and turbulence-enhanced velocity dispersions of gas-rich discs. Theorists have interpreted kinematic signatures of galaxies in a variety of ways (rotation, merging, outflows, and feedback) and attempted to discuss evolution vs. theoretical models and relate it to the evolution in galaxy morphology. A key point that has emerged from this activity is that substantial fractions of high-redshift galaxies have regular kinematic morphologies despite irregular photometric morphologies and this is likely due to the presence of a large number of highly gas-rich discs. There has not yet been a review of this burgeoning topic. In this first Dawes review, I will discuss the extensive kinematic surveys that have been done and the physical models that have arisen for young galaxies at high-redshift.

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“…GPs are star-forming galaxies which receive this name because of their compactness and green color in SDSS composite images (Cardamone et al 2009). The color is produced by an unusually large [OIII]λ5007 Å emission line redshifted so as to contribute to the g-band color.…”

Section: Nitrogen and Oxygen In Green-pea (Gp) Galaxiesmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

183

130

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Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

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Galaxy Zoo Green Peas: discovery of a class of compact extremely star-forming galaxies

Cited by 581 publications

References 107 publications

Ly$\mathsf{\alpha}$ emitters in the GOODS-S field

Ly$\mathsf{\alpha}$ emitters in the GOODS-S field

The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time

Star formation sustained by gas accretion

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