Quantifying the Effect of Field Variance on the Hα Luminosity Function with the New Numerical Galaxy Catalog (ν<sup>2</sup>GC)

Ogura, K.; Nagashima, Masahiro; Shimakawa, Rhythm; Hayashi, Masao; Kobayashi, Masakazu A. R.; Oogi, Taira; Ishiyama, Tomoaki; Koyama, Yusei; Makiya, Ryu; Okoshi, Katsuya; Onodera, Makoto; Shirakata, Hikari

doi:10.3847/1538-4357/ab8631

Cited by 5 publications

(4 citation statements)

References 84 publications

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“…For the observed Hα LFs (figure 10), the faint end slope is flatter than the PDR1 result as well as the results from the other previous studies, which makes the observed LF more consistent with the LF expected from a semi-analytic model (Ogura et al 2020). For the observed [OIII] LFs (figure 11), the number density is larger than that of the PDR1 LF.…”

Section: Emission-line Luminosity Functionssupporting

confidence: 74%

“…The ∼ 10 deg 2 NB imaging surveys by Sobral et al (2015) and Stroe & Sobral (2015) show that a large survey volume of >3.5-5.0×10 5 Mpc 3 can overcome cosmic variance and then the luminosity functions of emission-line galaxies are derived with an error of < 10%. From a theoretical point of view, Ogura et al (2020) investigate the influence of the field variance in Hα emission-line galaxies at z = 0.4 using a semi-analytic model for the galaxy formation, the New Numerical Galaxy Catalog (ν 2 GC), and find that a survey area of more than 15 deg 2 is required to restrict the uncertainties in the luminosity functions of Hα emitters at z = 0.4 to less than ∼ 10%.…”

Section: Introductionmentioning

confidence: 99%

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A 16 deg$^2$ survey of emission-line galaxies at z<1.6 from HSC-SSP PDR2 and CHORUS

Hayashi,

Shimakawa,

Tanaka

et al. 2020

Preprint

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We have conducted a comprehensive survey of emission-line galaxies at z < ∼ 1.6 based on narrowband (NB) imaging data taken with Hyper Suprime-Cam (HSC) on the Subaru telescope. In this paper, we update the catalogs of Hα, [OIII], and [OII] emission-line galaxies using the data from the second Public Data Release (PDR2) of Subaru Strategic Program (SSP) of HSC and Cosmic HydrOgen Reionization Unveiled with Subaru (CHORUS) survey along with the spectroscopic redshifts for 2,019 emission-line galaxies selected with the PDR1 data. The wider effective coverage of NB816 and NB921, 16.3 deg 2 and 16.9 deg 2 respectively, are available in the Deep and UltraDeep layers of HSC-SSP from the PDR2. The CHORUS survey provides us with data with additional three NBs (NB527, NB718, and NB973) in the COSMOS field in the UltraDeep layer (1.37 deg 2 ). The five NB datasets allow us to investigate the starforming galaxies presenting emission-lines at 14 specific redshifts ranging from z ∼ 1.6 down to z ∼ 0.05. We revisit the distribution of large-scale structures and luminosity functions (LFs) for the emission-line galaxies with the large samples of 75,377 emission-line galaxies selected. The redshift revolution of LFs shows that the star formation rate densities (SFRDs) decreases monotonically from z ∼ 1.6, which is consistent with the cosmic SFRD ever known. Our samples of emission-line galaxies covering a sufficiently large survey volume are useful to investigate the evolution of star-forming galaxies since the cosmic noon in a wide range of environments including galaxy clusters, filaments, and voids.

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Section: Emission-line Luminosity Functionssupporting

confidence: 74%

Section: Introductionmentioning

confidence: 99%

A 16 deg$^2$ survey of emission-line galaxies at z<1.6 from HSC-SSP PDR2 and CHORUS

Hayashi,

Shimakawa,

Tanaka

et al. 2020

Preprint

Self Cite

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“…A number of studies have theoretically evaluated the cosmic variance of galaxies at high redshift (e.g. Somerville et al 2004;Trenti & Stiavelli 2008;Ogura et al 2020;Bhowmick et al 2020;Ucci et al 2021). Ogura et al (2020) used a semi-analytic model of galaxy and AGN formation, the New Numerical Galaxy Catalog (ν 2 GC; Makiya et al 2016;Shirakata et al 2019), to evaluate the cosmic variance of Hα emitters at z = 0.4.…”

Section: Introductionmentioning

confidence: 99%

“…Somerville et al 2004;Trenti & Stiavelli 2008;Ogura et al 2020;Bhowmick et al 2020;Ucci et al 2021). Ogura et al (2020) used a semi-analytic model of galaxy and AGN formation, the New Numerical Galaxy Catalog (ν 2 GC; Makiya et al 2016;Shirakata et al 2019), to evaluate the cosmic variance of Hα emitters at z = 0.4. They also quantified how cosmic variance depends on survey volume.…”

Section: Introductionmentioning

confidence: 99%

Uchuu-$ν^2$GC galaxies and AGN: Cosmic variance forecasts of high-redshift AGN for JWST, Euclid, and LSST

Oogi¹,

Ishiyama²,

Prada³

et al. 2022

Preprint

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Measurements of the luminosity function of active galactic nuclei (AGN) at high redshift (z 6) are expected to suffer from field-to-field variance, including cosmic and Poisson variances. Future surveys, such as those from the Euclid telescope and James Webb Space Telescope (JWST), will also be affected by field variance. We use the Uchuu simulation, a state-of-the-art cosmological N -body simulation with 2.1 trillion particles in a volume of 25.7 Gpc 3 , that has sufficient mass resolution to resolve dwarf-size systems, combined with a semi-analytic galaxy and AGN formation model, to generate the Uchuu-ν 2 GC catalog, publicly available, that allows us to investigate the field-to-field variance of the luminosity function of AGN. With this Uchuu-ν 2 GC model, we quantify the cosmic variance as a function of survey area, AGN luminosity, and redshift. In general, cosmic variance decreases with increasing survey area and decreasing redshift. We find that at z ∼ 6 − 7, the cosmic variance depends weakly on AGN luminosity, in particular for small survey areas (0.01 and 0.1 deg 2 ). This is because the typical mass of dark matter haloes in which AGN reside does not significantly depend on luminosity. Due to the rarity of AGN, Poisson variance dominates the total field-to-field variance, especially for bright AGN. We also examine the effect of parameters related to galaxy formation physics on the field variance. We discuss uncertainties present in the estimation of the faint-end of the AGN luminosity function from recent observations, and extend this to make predictions for the expected number of AGN and their variance for upcoming observations with Euclid, JWST, and the Legacy Survey of Space and Time (LSST). In particular, we predict that the Euclid deep survey will find 120-240 (16-80) AGN -depending on the model -with rest-frame UV absolute magnitude brighter than −20 (−20.5) at z = 6.3 (z = 7) in the Euclid H-band deep survey. For the Euclid wide survey, we predict 15000-45000 (3000-15000) AGN with UV magnitude brighter than −22 (−22.5) will be detectable at z = 6.3 (z = 7).

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Impact of photochemical hazes and gases on exoplanet atmospheric thermal structure

Lavvas

Arfaux

2021

Monthly Notices of the Royal Astronomical Society

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We investigate the impact of photochemical hazes and disequilibrium gases on the thermal structure of hot-Jupiters, using a detailed 1-D radiative-convective model. We find that the inclusion of photochemical hazes results in major heating of the upper and cooling of the lower atmosphere. Sulphur containing species, such as SH, S2 and S3 provide significant opacity in the middle atmosphere and lead to local heating near 1 mbar, while OH, CH, NH, and CN radicals produced by the photochemistry affect the thermal structure near 1 μbar. Furthermore we show that the modifications on the thermal structure from photochemical gases and hazes can have important ramifications for the interpretation of transit observations. Specifically, our study for the hazy HD 189733 b shows that the hotter upper atmosphere resulting from the inclusion of photochemical haze opacity imposes an expansion of the atmosphere, thus a steeper transit signature in the UV-Visible part of the spectrum. In addition, the temperature changes in the photosphere also affect the secondary eclipse spectrum. For HD 209458 b we find that a small haze opacity could be present in this atmosphere, at pressures below 1 mbar, which could be a result of both photochemical hazes and condensates. Our results motivate the inclusion of radiative feedback from photochemical hazes in general circulation models for a proper evaluation of atmospheric dynamics.

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Quantifying the Effect of Field Variance on the Hα Luminosity Function with the New Numerical Galaxy Catalog (ν²GC)

Cited by 5 publications

References 84 publications

A 16 deg$^2$ survey of emission-line galaxies at z<1.6 from HSC-SSP PDR2 and CHORUS

A 16 deg$^2$ survey of emission-line galaxies at z<1.6 from HSC-SSP PDR2 and CHORUS

Uchuu-$ν^2$GC galaxies and AGN: Cosmic variance forecasts of high-redshift AGN for JWST, Euclid, and LSST

Impact of photochemical hazes and gases on exoplanet atmospheric thermal structure

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Quantifying the Effect of Field Variance on the Hα Luminosity Function with the New Numerical Galaxy Catalog (ν2GC)

Cited by 5 publications

References 84 publications

A 16 deg$^2$ survey of emission-line galaxies at z<1.6 from HSC-SSP PDR2 and CHORUS

A 16 deg$^2$ survey of emission-line galaxies at z<1.6 from HSC-SSP PDR2 and CHORUS

Uchuu-$ν^2$GC galaxies and AGN: Cosmic variance forecasts of high-redshift AGN for JWST, Euclid, and LSST

Impact of photochemical hazes and gases on exoplanet atmospheric thermal structure

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Quantifying the Effect of Field Variance on the Hα Luminosity Function with the New Numerical Galaxy Catalog (ν²GC)