scholarly journals The z ∼ 2 [O iii] Luminosity Function of Grism-selected Emission-line Galaxies

2021 ◽  
Vol 920 (2) ◽  
pp. 78
Author(s):  
William P. Bowman ◽  
Robin Ciardullo ◽  
Gregory R. Zeimann ◽  
Caryl Gronwall ◽  
Donghui Jeong ◽  
...  
Keyword(s):  
Emission Line ◽  
Luminosity Function ◽  
Emission Line Galaxies

scholarly journals Prediction of H α and [O iii] emission line galaxy number counts for future galaxy redshift surveys

2019 ◽  
Vol 490 (3) ◽  
pp. 3667-3678 ◽  
Author(s):  
Zhongxu Zhai ◽  
Andrew Benson ◽  
Yun Wang ◽  
Gustavo Yepes ◽  
Chia-Hsun Chuang
Keyword(s):  
Emission Line ◽  
Galaxy Formation ◽  
Luminosity Function ◽  
Large Scale ◽  
High Redshift ◽  
Flux Ratio ◽  
Formation Model ◽  
Line Flux ◽  
Emission Line Galaxies ◽  
Number Counts

ABSTRACT We perform a simulation with Galacticus, a semi-analytical galaxy formation model, to predict the number counts of H α and [O iii] emitting galaxies. With a state-of-the-art N-body simulation, UNIT, we first calibrate Galacticus with the current observation of H α luminosity function. The resulting model coupled with a dust attenuation model, can reproduce the current observations, including the H α luminosity function from HiZELS and number density from WISP. We extrapolate the model prediction to higher redshift and the result is found to be consistent with previous investigations. We then use the same galaxy formation model to predict the number counts for [O iii] emitting galaxies. The result provides further validation of our galaxy formation model and dust model. We present number counts of H α and [O iii] emission line galaxies for three different line flux limits: 5 × 10−17erg s−1 cm−2, 1 × 10−16 erg s−1 cm−2 (6.5σ nominal depth for WFIRST GRS), and 2 × 10−16 erg s−1 cm−2 (3.5σ depth of Euclid GRS). At redshift 2 < z < 3, our model predicts that WFIRST can observe hundreds of [O iii] emission line galaxies per square degree with a line flux limit of 1 × 10−16 erg s−1 cm−2. This will provide accurate measurement of large-scale structure to probe dark energy over a huge cosmic volume to an unprecedented high redshift. Finally, we compare the flux ratio of H α/[O iii] within the redshift range of 0 < z < 3. Our results show the known trend of increasing H α/[O iii] flux ratio with H α flux at low redshift, which becomes a weaker trend at higher redshifts.

scholarly journals Luminosity function of [O ii] emission-line galaxies in the MassiveBlack-II simulation

2015 ◽  
Vol 454 (1) ◽  
pp. 277-287 ◽  
Author(s):  
KwangHo Park ◽  
Tiziana Di Matteo ◽  
Shirley Ho ◽  
Rupert Croft ◽  
Stephen M. Wilkins ◽  
...  
Keyword(s):  
Emission Line ◽  
Luminosity Function ◽  
Emission Line Galaxies

A Study of the [OII]λ3727/Hα Flux Ratio of Emission Line Galaxies

2010 ◽  
Vol 34 (3) ◽  
pp. 234-244 ◽  
Author(s):  
Gao Feng ◽  
Kong Xu ◽  
Lin Xuan-bin ◽  
Zhang Wei ◽  
Li Jun-rong
Keyword(s):  
Emission Line ◽  
Flux Ratio ◽  
Emission Line Galaxies

scholarly journals Extreme emission-line galaxies out toz~ 1 in zCOSMOS

2015 ◽  
Vol 578 ◽  
pp. A105 ◽  
Author(s):  
R. Amorín ◽  
E. Pérez-Montero ◽  
T. Contini ◽  
J. M. Vílchez ◽  
M. Bolzonella ◽  
...  
Keyword(s):  
Emission Line ◽  
Emission Line Galaxies

scholarly journals The completed SDSS-IV extended baryon oscillation spectroscopic survey: growth rate of structure measurement from anisotropic clustering analysis in configuration space between redshift 0.6 and 1.1 for the emission-line galaxy sample

2020 ◽  
Vol 499 (4) ◽  
pp. 5527-5546 ◽  
Author(s):  
Amélie Tamone ◽  
Anand Raichoor ◽  
Cheng Zhao ◽  
Arnaud de Mattia ◽  
Claudio Gorgoni ◽  
...  
Keyword(s):  
Growth Rate ◽  
Correlation Function ◽  
Emission Line ◽  
Sloan Digital Sky Survey ◽  
Linear Growth Rate ◽  
Angular Diameter Distance ◽  
Consensus Values ◽  
Galaxy Sample ◽  
Emission Line Galaxies ◽  
Anisotropic Clustering

ABSTRACT We present the anisotropic clustering of emission-line galaxies (ELGs) from the Sloan Digital Sky Survey IV (SDSS-IV) extended Baryon Oscillation Spectroscopic Survey (eBOSS) Data Release 16 (DR16). Our sample is composed of 173 736 ELGs covering an area of 1170 deg2 over the redshift range 0.6 ≤ z ≤ 1.1. We use the convolution Lagrangian perturbation theory in addition to the Gaussian streaming redshift space distortions to model the Legendre multipoles of the anisotropic correlation function. We show that the eBOSS ELG correlation function measurement is affected by the contribution of a radial integral constraint that needs to be modelled to avoid biased results. To mitigate the effect from unknown angular systematics, we adopt a modified correlation function estimator that cancels out the angular modes from the clustering. At the effective redshift, zeff = 0.85, including statistical and systematical uncertainties, we measure the linear growth rate of structure fσ8(zeff) = 0.35 ± 0.10, the Hubble distance $D_ H(z_{\rm eff})/r_{\rm drag} = 19.1^{+1.9}_{-2.1}$, and the comoving angular diameter distance DM(zeff)/rdrag = 19.9 ± 1.0. These results are in agreement with the Fourier space analysis, leading to consensus values of: fσ8(zeff) = 0.315 ± 0.095, $D_H(z_{\rm eff})/r_{\rm drag} = 19.6^{+2.2}_{-2.1}$, and DM(zeff)/rdrag = 19.5 ± 1.0, consistent with ΛCDM model predictions with Planck parameters.

scholarly journals Spectral classification of emission-line galaxies

1987 ◽  
Vol 63 ◽  
pp. 295 ◽  
Author(s):  
Sylvain Veilleux ◽  
Donald E. Osterbrock
Keyword(s):  
Emission Line ◽  
Spectral Classification ◽  
Emission Line Galaxies

scholarly journals The Hamburg/SAO survey for emission–line galaxies

1999 ◽  
Vol 137 (2) ◽  
pp. 299-304 ◽  
Author(s):  
S. A. Pustilnik ◽  
D. Engels ◽  
A. V. Ugryumov ◽  
V. A. Lipovetsky ◽  
H.-J. Hagen ◽  
...  
Keyword(s):  
Emission Line ◽  
Emission Line Galaxies

scholarly journals Low Metallicity Galaxies at z ~ 0.7: Keys to the Origins of Metallicity Scaling Laws

2008 ◽  
Vol 4 (S255) ◽  
pp. 397-401
Author(s):  
David J. Rosario ◽  
Carlos Hoyos ◽  
David Koo ◽  
Andrew Phillips
Keyword(s):  
Star Formation ◽  
Emission Line ◽  
Galaxy Evolution ◽  
Scaling Laws ◽  
Temperature Sensitive ◽  
Star Forming ◽  
Low Metallicity ◽  
Emission Line Galaxies ◽  
Halo Masses ◽  
Stellar Masses

AbstractWe present a study of remarkably luminous and unique dwarf galaxies at redshifts of 0.5 < z < 0.7, selected from the DEEP2 Galaxy Redshift survey by the presence of the temperature sensitive [OIII]λ4363 emission line. Measurements of this important auroral line, as well as other strong oxygen lines, allow us to estimate the integrated oxygen abundances of these galaxies accurately without being subject to the degeneracy inherent in the standard R23 system used by most studies. [O/H] estimates range between 1/5–1/10 of the solar value. Not surprisingly, these systems are exceedingly rare and hence represent a population that is not typically present in local surveys such as SDSS, or smaller volume deep surveys such as GOODS.Our low-metallicity galaxies exhibit many unprecedented characteristics. With B-band luminosities close to L*, thse dwarfs lie significantly away from the luminosity-metallicity relationships of both local and intermediate redshift star-forming galaxies. Using stellar masses determined from optical and NIR photometry, we show that they also deviate strongly from corresponding mass-metallicity relationships. Their specific star formation rates are high, implying a significant burst of recent star formation. A campaign of high resolution spectroscopic follow-up shows that our galaxies have dynamical properties similar to local HII and compact emission line galaxies, but mass-to-light ratios that are much higher than average star-forming dwarfs.The low metallicities, high specific star formation rates, and small halo masses of our galaxies mark them as lower redshift analogs of Lyman-Break galaxies, which, at z ~ 2 are evolving onto the metallicity sequence that we observe in the galaxy population of today. In this sense, these systems offer fundamental insights into the physical processes and regulatory mechanisms that drive galaxy evolution in that epoch of major star formation and stellar mass assembly.

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