SDSS-IV eBOSS emission-line galaxy pilot survey

Comparat, Johan; Delubac, Timothée; Jouvel, S.; Raichoor, Anand; Kneib, Jean-Paul; Yèche, Ch; Abdalla, F. B.; Cras, Claire Le; Maraston, Claudia; Wilkinson, David M.; Zhu, Guangtun; Jullo, Eric; Prada, Francisco; Schlegel, David J.; Xu, Zhilei; Zou, Hu; Bautista, Julian; Bizyaev, Dmitry; Bolton, A.; Brownstein, Joel R.; Dawson, Kyle; Escoffier, S.; Gaulme, P.; Kinemuchi, Karen; Malanushenko, Elena; Malanushenko, Viktor; Vivek, M.; Newman, Jeffrey A.; Oravetz, Daniel; Pan, Kaike; Percival, Will J.; Prakash, Abhishek; Schneider, D.; Simmons, A.; Abbott, T. M. C.; Allam, S.; Banerji, M.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Capozzi, D.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Cunha, C. E.; Costa, L. N. da; Desai, S.; Doel, P.; Eifler, T. F.; Estrada, J.; Flaugher, B.; Fosalba, P.; Frieman, Joshua A.; Gaztañaga, E.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gutiérrez, G.; Honscheid, K.; James, D. J.; Kuêhn, K.; Kuropatkin, N.; Lahav, O.; Lima, M.; Maia, M. A. G.; March, M.; Marshall, J. L.; Miquel, R.; Plazas, A. A.; Reil, K.; Roe, Natalie A.; Romer, A. K.; Roodman, A.; Rykoff, E. S.; Šako, M.; Sánchez, E.; Scarpine, V.; Sevilla-Noarbe, I.; Soares-Santos, M.; Sobreira, F.; Suchyta, E.; Swanson, M. E. C.; Tarlè, G.; Thaler, J. J.; Thomas, Daniel; Walker, A. R.; Zhang, Y.

doi:10.1051/0004-6361/201527377

Cited by 44 publications

(36 citation statements)

References 51 publications

(64 reference statements)

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“…For the type 1 AGNs, there exist a large number of optical spectra, and the stacking method permits the construction of high-quality stacks that are almost noise free, see Fig B1. For the type 2 AGNs, the number of available spectra is small, so that the stacks have noise, in particular at redshift higher than 1, see Fig B2. For the type 3 AGNs, we use the elliptical, red galaxy spectrum model, see Fig B3. To construct galaxy archetypes we use SDSS spectra as selected in (Abazajian et al 2009;Dawson et al 2013;Prakash et al 2016) for the elliptical galaxies ( Fig B3) and as in (Comparat et al 2013(Comparat et al , 2016Raichoor et al 2017) for the star-forming galaxies ( Fig B4).…”

Section: Optical Medium Resolution Spectramentioning

confidence: 99%

Active galactic nuclei and their large-scale structure: an eROSITA mock catalogue

Comparat

Merloni

Salvato

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In the context of the upcoming SRG/eROSITA survey, we present an N-body simulation-based mock catalogue for X-ray selected AGN samples. The model reproduces the observed hard X-ray AGN luminosity function (XLF) and the soft X-ray logN-logS from redshift 0 to 6. The XLF is reproduced to within ±5% and the logN-logS to within ±20%. We develop a joint X-ray -optical extinction and classification model. We adopt a set of empirical spectral energy distributions to predict observed magnitudes in the UV, optical and NIR. With the latest eROSITA all sky survey sensitivity model, we create a high-fidelity full-sky mock catalogue of X-ray AGN. It predicts their distributions in right ascension, declination, redshift and fluxes. Using empirical medium resolution optical spectral templates and an exposure time calculator, we find that 1.1×10 6 (4×10 5 ) fiber-hours are needed to follow-up spectroscopically from the ground the detected X-ray AGN with an optical magnitude 21 < r < 22.8 (22.8 < r < 25) with a 4-m (8-m) class multi-object spectroscopic facility. We find that future clustering studies will measure the AGN bias to the percent level at redshift z < 1.2 and should discriminate possible scenarios of galaxy-AGN co-evolution. We predict the accuracy to which the baryon acoustic oscillation standard ruler will be measured using X-ray AGN: better than 3% for AGN between redshift 0.5 to 3 and better than 1% using the Lyα forest of X-ray QSOs discovered between redshift 2 and 3. eROSITA will provide an outstanding set of targets for future galaxy evolution and cosmological studies.

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Section: Optical Medium Resolution Spectramentioning

confidence: 99%

Active galactic nuclei and their large-scale structure: an eROSITA mock catalogue

Comparat

Merloni

Salvato

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Though pilot surveys demonstrated that a target selection based on the SDSS imaging passed the eBOSS requirements (Comparat et al 2016a;Raichoor et al 2016;Delubac et al 2017), the deep grz-band photometry of the Dark Energy Camera Legacy Survey (DECaLS 15 ) enables a more efficient target selection. Thus, the eBOSS ELG target selection ) has been done on the DECaLS grz-band photometry.…”

Section: Eboss Elg Samplementioning

confidence: 99%

“…The number of observed high-redshift star-forming galaxies with emission line measurements is growing quickly with recent optical and near-infrared surveys (see e.g., Comparat et al 2016a;Okada et al 2016;Delubac et al 2017;Kaasinen et al 2017;Drinkwater et al 2018). But the sample sizes of the current ELG surveys are still not large enough to fully understand the properties of the high-redshift ELGs.…”

Section: Introductionmentioning

confidence: 99%

Evolution of Star-forming Galaxies from z = 0.7 to 1.2 with eBOSS Emission-line Galaxies

Guo¹,

Yang

Raichoor

et al. 2019

ApJ

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We study the evolution of star-forming galaxies with 10 10 M < M * < 10 11.6 M over the redshift range of 0.7 < z < 1.2 using the emission-line galaxies (ELGs) in the extended Baryon Oscillation Spectroscopic Survey (eBOSS). By applying the incomplete conditional stellar mass function (ICSMF) model proposed in Guo et al. (2018), we simultaneously constrain the sample completeness, the stellarhalo mass relation (SHMR) and the quenched galaxy fraction. We obtain the intrinsic stellar mass functions for star-forming galaxies in the redshift bins of 0.7 < z < 0.8, 0.8 < z < 0.9, 0.9 < z < 1.0 and 1.0 < z < 1.2, as well as the stellar mass function for all galaxies in the redshift bin of 0.7 < z < 0.8. We find that the eBOSS ELG sample only selects about 1%-10% of the star-forming galaxy population at the different redshifts, with the lower redshift samples to be more complete. There is only weak evolution in the SHMR of the ELGs from z = 1.2 to z = 0.7, as well as the intrinsic galaxy stellar mass functions. Our best-fitting models show that the central ELGs at these redshifts live in halos of mass M ∼ 10 12 M , while the satellite ELGs occupy slightly more massive halos of M ∼ 10 12.6 M . The average satellite fraction of the observed ELGs varies from 13% to 17%, with the galaxy bias increasing from 1.1 to 1.4 from z = 0.7 to 1.2.

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“…These surveys use the Sloan Foundation 2.5m Telescope at Apache Point Observatory (Gunn et al 2006), and the BOSS spectrograph, which covers the wavelength range of 360 ∼ 1000 nm with 1000 fibers per 7-deg 2 plate at a resolution of R ∼ 2000 (Smee et al 2013). The ELG target selection is based on grz-band photometry (Comparat et al 2016;Raichoor et al 2017) (Comparat et al 2013. The ELG survey covers an area of ∼ 620 deg 2 in the Southern Galactic Cap (SGC) and ∼ 600 deg 2 in the Northern Galactic Cap (NGC) at a target density of 200 deg −2 in the NGC and 240 deg −2 in the SGC, respectively.…”

Section: Eboss Survey and Elg Samplementioning

confidence: 99%

The Mass–Metallicity Relation at z ∼ 0.8: Redshift Evolution and Parameter Dependency

Huang

Zou

Kong

et al. 2019

ApJ

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The spectra of emission-line galaxies (ELGs) from the extended Baryon Oscillation Spectroscopic Survey (eBOSS) of the Sloan Digit Sky Survey (SDSS) are used to study the mass-metallicity relation (MZR) at z ∼ 0.8. The selected sample contains about 180,000 massive star-forming galaxies with 0.6 < z < 1.05 and 9 < log(M ⋆ /M ⊙ ) < 12. The spectra are stacked in bins of different parameters including redshift, stellar mass, star formation rate (SFR), specific star formation rate (sSFR), halflight radius, mass density, and optical color. The average MZR at z ∼ 0.83 has a downward evolution in the MZR from local to high-redshift universe, which is consistent with previous works. At a specified stellar mass, galaxies with higher SFR/sSFR and larger half-light radius have systematically lower metallicity. This behavior is reversed for galaxies with larger mass density and optical color. Among the above physical parameters, the MZR has the most significant dependency on SFR. Our galaxy sample at 0.6 < z < 1.05 approximately follows the fundamental metallicity relation (FMR) in the local universe, although the sample inhomogeneity and incompleteness might have effect on our MZR and FMR.

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SDSS-IV eBOSS emission-line galaxy pilot survey

Cited by 44 publications

References 51 publications

Active galactic nuclei and their large-scale structure: an eROSITA mock catalogue

Active galactic nuclei and their large-scale structure: an eROSITA mock catalogue

Evolution of Star-forming Galaxies from z = 0.7 to 1.2 with eBOSS Emission-line Galaxies

The Mass–Metallicity Relation at z ∼ 0.8: Redshift Evolution and Parameter Dependency

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