adsabs/AstroCLIMB huggingface dataset:
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Rest-frame UV luminosity functions of all rest-UV selected sources (galaxies+AGNs) at z ∼ 3, 4, 5, 6, and 7 from top to bottom. The red circles show our results based on the HSC-SSP survey data at z ∼ 4–7 and results in Moutard et al. (2020) at z ∼ 3. The magenta squares and orange diamonds are results for galaxies taken from Bouwens et al. (2021) and Ishigaki et al. (2018), respectively. The orange squares are results for AGNs in Zhang et al. (2021), Akiyama et al. (2018), Niida et al. (2020), and Matsuoka et al. (2018c) at MUV < −24 mag. The blue (green) lines show the best-fit DPL+DPL (DPL+Schechter) functions. Note that at z ∼ 7, we fix the parameter of the AGN luminosity function to values in Matsuoka et al. (2018c), except for the ϕ* parameter that is decreased by 0.7 dex from Matsuoka et al.’s value following ϕ* ∝ 10−0.7(z−6) as assumed in Matsuoka et al. (2018c).
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Evolution of the rest-frame UV luminosity functions of all rest-UV selected sources (galaxies+AGNs) from z ∼ 7 to z ∼ 0. The bottom panel shows the luminosity functions at z ∼ 0–7, and the black, gray, brown, purple, blue, green, orange, and red symbols show results at z ∼ 0.2, 1, 2, 3, 4, 5, 6, and 7, respectively. The circles at z ∼ 4–7 show our results based on the HSC-SSP survey data, and those at z ∼ 0–3 are taken from Moutard et al. (2020) at 0.05 < z < 0.3, 0.9 < z < 1.3, 1.8 < z < 2.5, and 2.5 < z < 3.5. The diamonds are results for AGNs in Zhang et al. (2021), Akiyama et al. (2018), Niida et al. (2020), and Matsuoka et al. (2018c) at z ∼ 3, 4, 5, and 6, respectively, and the squares show results for galaxies in Bouwens et al. (2021) and Ishigaki et al. (2018). The lines show the best-fit DPL+DPL functions at z ∼ 3–7 (this study), and Schechter functions at z ∼ 0–2 (Moutard et al. 2020). The top panel shows ratios of the number densities at z ∼ 3–5 relative to those at z ∼ 6. The shaded regions correspond to the 2σ uncertainties of the luminosity function parameters. The number density of typical galaxies (﹩{M}_{\mathrm{UV}}={M}_{\mathrm{UV}}^{* }\sim -21﹩ mag) increases only by a factor of ∼3 from z ∼ 6 to 3, while the number density of typical quasars (﹩{M}_{\mathrm{UV}}={M}_{\mathrm{UV}}^{* }\sim -27﹩ mag) significantly increases by a factor of ∼100.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Spectroscopic galaxy fraction at z ∼ 4. The black circles are those estimated by using the all available spectroscopic catalogs (same as the top panel of Figure 5), and the red circles are those estimated with the VVDS data (Le Fèvre et al. 2013).
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Rest-frame UV luminosity functions of galaxies that take into account AGN fraction correction at z ∼ 4, 5, 6, and 7, from top to bottom. The red line is the best-fit DPL function, and the green line is the best-fit Schechter function without considering the lensing effect. The blue shaded region corresponds to the lensed Schechter functions with the two cases of optical depth estimates (Takahashi et al. 2011 and Barone-Nugent et al. 2015). The red circles show our results based on the HSC-SSP survey data. The magenta squares and orange diamonds are results for galaxies taken from Bouwens et al. (2021) and Ishigaki et al. (2018), respectively.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Evolution of the rest-frame UV luminosity functions of galaxies from z ∼ 10 to z ∼ 4. The bottom panel shows the luminosity functions at z ∼ 4–10, and the blue, green, orange, red, magenta, purple, and pink symbols show results at z ∼ 4, 5, 6, 7, 8, 9, and 10, respectively. The circles at z ∼ 4–7 show our results based on the HSC-SSP survey data, and those at z ∼ 8–10 are taken from Bowler et al. (2020). The squares show results for galaxies in Bouwens et al. (2021). The lines show the best-fit DPL functions in this study at z ∼ 4–7 and Bowler et al. (2020) at z ∼ 8–10. The top panel shows ratios of the number densities relative to those at z ∼ 10. The shaded regions at z ∼ 4–7 correspond to the 2σ uncertainties of the luminosity function parameters. The number density of typical galaxies (﹩{M}_{\mathrm{UV}}={M}_{\mathrm{UV}}^{* }\sim -21﹩ mag) significantly increases by a factor of ∼100 from ∼10 to 4, while that of faint galaxies (MUV ∼ −16 mag) mildly increases by a factor of ∼10. The number density of the bright galaxies at −25 ≲ MUV ≲ −23 mag does not significantly change at z ∼ 4–10.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Obtained angular correlation functions of the subsamples and their best fit by the HOD models at z ∼ 1.7, 2.2, and 3. The black squares denote the angular correlation function of the subsample at each redshift. The data denoted by the open squares are not used in our HOD model fitting because they are at too-small scales or possibly affected by the nonlinear halo bias effect. The dashed and dotted–dashed lines represent the one-halo and two-halo terms, respectively, and the solid line is the summations of the one-halo and two-halo terms.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Same as Figure 12 but at z ∼ 4, 5, and 6.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Comparisons of the angular correlation functions with the literature. The black squares represent the correlation functions in this study. The open circles, squares, and diamonds denote results in Adelberger et al. (2005), Savoy et al. (2011), and Hildebrandt et al. (2009), respectively. Our obtained measurements agree well with these previous studies.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Comparison of the number densities between the HOD models and observations. The gray, brown, purple, blue, green, orange, and red squares (circles) represent the relative differences of the number densities between the HOD models and observations for the subsamples in this work (in Harikane et al. 2016), at z ∼ 1.7, 2.2, 3, 4, 5, 6, and 7, respectively, as a function of the threshold absolute UV magnitudes, ﹩{M}_{\mathrm{UV}}^{\mathrm{th}}﹩.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: MUV–Mh relation. The gray, brown, purple, blue, green, orange, and red filled diamonds (circles) denote the halo masses as a function of the UV magnitude at z ∼ 1.7, 2.2, 3, 4, 5, 6, and 7, respectively, for the subsamples in this work (in Harikane et al. 2016). We plot ﹩{M}_{\min }﹩ and ﹩{M}_{\mathrm{UV}}^{\mathrm{th}}﹩ as Mh and MUV, respectively. The crosses are results of the previous work based on the early HSC-SSP data (Harikane et al. 2018b). The solid curves show the best-fit relations of Equation (54).
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Comparison of the mean dark matter halo masses, ﹩\left\langle {M}_{{\rm{h}}}\right\rangle ﹩, with the literature under the same cosmology. We plot ﹩{M}_{\mathrm{UV}}^{\mathrm{th}}﹩ as MUV. The diamonds represent the mean dark matter halo masses in this work with the cosmological parameters of (h, Ωm, ΩΛ, σ8) = (0.7, 0.3, 0.7, 0.9). The circles are the results of Harikane et al. (2016) with the same cosmology. The black symbols denote results of the previous studies. We plot the results of Hildebrandt et al. (2009; squares), Lee et al. (2006; upward triangles), Ouchi et al. (2005; stars), and Hamana et al. (2004; downward triangle). The downward triangles have no error bars, because Hamana et al. (2004) do not provide errors of the mean dark matter halo mass. We also show the results of Barone-Nugent et al. (2014) as black open squares, which are recalculated with the cosmological parameters of (h, Ωm, ΩL, σ8) = (0.7, 0.3, 0.7, 0.9). The mean dark matter halo mass of the faintest subsample at z ∼ 3 is slightly more massive than that of the next faintest subsample, because of the higher fraction of satellite galaxies that are typically residing in massive halos (see Table 8).
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption:  ﹩\mathrm{SFR}/{\dot{{M}}}_{{\rm{h}}}﹩ and baryon conversion efficiency (﹩\mathrm{SFR}/({{f}}_{{b}}{\dot{{M}}}_{{\rm{h}}})﹩) as a function of the halo mass. The gray, brown, purple, blue, green, orange, and red filled diamonds (circles) denote the ratios as a function of the halo mass, at z ∼ 1.7, 2.2, 3, 4, 5, 6, and 7, respectively, for the subsamples in this work (in Harikane et al. 2016). The statistical errors for our data are smaller than the symbols (diamonds). The black solid curve is the fitting formulae of Equation (56) for the ﹩\mathrm{SFR}/{\dot{M}}_{{\rm{h}}}\mbox{--}{M}_{{\rm{h}}}﹩ relation at z ∼ 2–7, and the gray shaded region represents the 2σ typical scatter (0.3 dex) of the data points compared to the relation.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Comparison of the ﹩\mathrm{SFR}/{\dot{{M}}}_{{\rm{h}}}﹩ ratio with the literature. The red solid curve shows the redshift-dependent relation constrained in this work (Equation (57)), and the shaded region represents the 2σ typical uncertainties. Results compared include those from our previous work: Equation (25) in Harikane et al. (2018a; red dashed curve), Behroozi et al. (2019; blue solid curve), Moster et al. (2018; gray dashed curve), Tacchella et al. (2018; green solid curve), Mason et al. (2015a; gray dotted curve), and Behroozi et al. (2013; blue dashed curve). All results are converted to use the Salpeter (1955) IMF (Equation (55)). The result of Harikane et al. (2018a) is recalculated based on the accretion rate of Behroozi & Silk (2015), and thus is ∼2 times higher than the original relation in Harikane et al. (2018a).
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Cosmic SFR density. The bottom panel shows the comparison of the cosmic SFR densities. The red curves with the shade represent cosmic SFR densities derived from Equation (58). For the solid and dashed lines, we assume the redshift-dependent and independent ﹩\mathrm{SFR}/{\dot{M}}_{{\rm{h}}}\mbox{--}{M}_{{\rm{h}}}﹩ relations (Equations (57) and (56)), respectively, which are constrained in this paper at 2 ≲ z ≲ 7. The shaded regions correspond to the 1σ (0.15 dex) scatter in the ﹩\mathrm{SFR}/{\dot{M}}_{{\rm{h}}}\mbox{--}{M}_{{\rm{h}}}﹩ relation. We integrate down to the halo mass corresponding to the SFR of 0.3 M⊙yr−1 (MUV = − 17 mag with the Madau & Dickinson 2014 calibration), as previous studies (Bouwens et al. 2015, 2020; Finkelstein et al. 2015b; Oesch et al. 2018). The black circles show observed cosmic SFR densities taken from Madau & Dickinson (2014), Finkelstein et al. (2015b), McLeod et al. (2016), and Bouwens et al. (2020). All results are converted to use the calibration of Madau & Dickinson (2014) with the Salpeter (1955) IMF (Equation (55)). The top panel shows ﹩{\rm{\Delta }}\tfrac{{\rm{S}}{\rm{F}}{\rm{R}}}{{\dot{M}}_{{\rm{h}}}}=\tfrac{{\rm{S}}{\rm{F}}{\rm{R}}}{{\dot{M}}_{{\rm{h}}}}(z)/\tfrac{{\rm{S}}{\rm{F}}{\rm{R}}}{{\dot{M}}_{{\rm{h}}}}(z=8)﹩ at a given halo mass. The sold and dashed curves are calculated with Equations (57) and (56), respectively.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Mechanism of the cosmic SFR density evolution. Top panel: the purple, blue, green, orange, and red curves indicate the number density of halos whose masses are Mh = 1010, 1011, 1012, 1013, and 1014 M⊙, respectively. The number density is calculated by using the Behroozi et al. (2013) halo mass function. The black curve represents a weighted number density based on Equation (57). Middle panel: same as the top panel but for the dark matter accretion rate calculated by using the formula in Behroozi & Silk (2015). Bottom panel: same as the top panel but for the cosmic SFR density. The gray circles are observed cosmic SFR densities taken from Madau & Dickinson (2014), Finkelstein et al. (2015b), McLeod et al. (2016), and Bouwens et al. (2020). Since the cosmic SFR density at a given halo mass is proportional to the galaxy (halo) number densities and SFRs (accretion rates) as shown in Equation (58), the redshift evolution of the cosmic SFR density is made by the monotonic steep increase of the halo number density from z ∼ 10 to z ∼ 4 and the monotonic decrease of the accretion rate from z ∼ 2 to z ∼ 0, resulting a peak of the SFR density around z ∼ 2–3.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Comparison of the rest-frame UV luminosity functions. Solid curves are the calculated luminosity functions from Equation (59) with the ﹩\mathrm{SFR}/{\dot{{M}}}_{{\rm{h}}}\mbox{--}{{M}}_{{\rm{h}}}﹩ relation of Equation (57). The points show the observed galaxy luminosity functions of Bouwens et al. (2021; circles), Moutard et al. (2020; squares), and Arnouts et al. (2005; stars). The shaded regions correspond to the 1σ (0.15 dex) scatter in the ﹩\mathrm{SFR}/{\dot{M}}_{{\rm{h}}}\mbox{--}{M}_{{\rm{h}}}﹩ relation.
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Comparison of the cosmic SFR density at z > 7. The red curve with the shade represents the cosmic SFR density calculated in this work based on the constant star formation efficiency at z > 5 (Equation (57)), integrated down to the SFR of 0.3 M⊙yr−1 (MUV = −17 mag), as previous studies (Bouwens et al. 2015, 2020; Finkelstein et al. 2015b; Oesch et al. 2018). The gray dashed curve shows the extrapolation of the relation of Madau & Dickinson (2014) at z > 6. The other curves show predictions from models of Mason et al. (2015a; blue dashed curve), Mashian et al. (2016; orange dashed curve), Sun & Furlanetto (2016; green solid curve), Tacchella et al. (2018; green dashed curve), and Behroozi et al. (2020; blue solid curve). The orange shaded region indicates a prediction of the halo evolution model in Oesch et al. (2018). All results are converted to use the Salpeter (1955) IMF (Equation (55)).
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Fit to the observed cosmic SFR densities. The red dashed curve represents our fit (Equation (60)) to the observed cosmic SFR densities at z ≲ 10 and the calculated SFR densities at z > 10 in this work. The gray dashed curve shows the fit in Madau & Dickinson (2014). All results are converted to use the Salpeter (1955) IMF (Equation (55)).
Paper: GOLDRUSH. IV. Luminosity Functions and Clustering Revealed with ∼4,000,000 Galaxies at z ∼ 2–7: Galaxy–AGN Transition, Star Formation Efficiency, and Implication for Evolution at z > 10
Authors: Yuichi Harikane, Yoshiaki Ono, Masami Ouchi, Chengze Liu, Marcin Sawicki, Takatoshi Shibuya, Peter S. Behroozi, Wanqiu He, Kazuhiro Shimasaku, Stephane Arnouts, Jean Coupon, Seiji Fujimoto, Stephen Gwyn, Jiasheng Huang, Akio K. Inoue, Nobunari Kashikawa, Yutaka Komiyama, Yoshiki Matsuoka, and Chris J. Willott
Figure caption: Cumulative number of formed stars as a function of the redshift. The red line shows the cumulative number of formed stars calculated based on the SFR density (Equation (61)). We extrapolate the ﹩\mathrm{SFR}/{\dot{M}}_{{\rm{h}}}\mbox{--}{M}_{{\rm{h}}}﹩ relation both to the higher-redshift and lower-mass range, and the shaded region indicates possible uncertainties of the ﹩\mathrm{SFR}/{\dot{M}}_{{\rm{h}}}﹩ ratio and the mass limit of the integration. The cumulative number reaches 1 around z ∼ 16–27, implying the first star formation at this epoch.