SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 &lt; z &lt; 6.9<sup>∗</sup>

†

Matsuoka, Yoshiki; Onoue, Masafusa; Kashikawa, Nobunari; Iwasawa, K.; Strauss, Michael A.; Nagao, Tohru; Imanishi, Masatoshi; Niida, Mana; Toba, Yoshiki; Akiyama, Masayuki; Asami, Naoko; Bosch, James; Foucaud, S.; Furusawa, Hisanori; Goto, Tomotsugu; Gunn, James E.; Harikane, Yuichi; Ikeda, Hiroyuki; Kawaguchi, Toshihiro; Kikuta, Satoshi; Komiyama, Yutaka; Lupton, Robert H.; Minezaki, Takeo; Miyazaki, Satoshi; Morokuma, Tomoki; Murayama, Hitoshi; Nishizawa, Atsushi J.; Ono, Yoshiyasu; Ouchi, Masami; Price, P. A.; Sameshima, Hiroaki; Silverman, John D.; Sugiyama, Naoshi; Tait, Philip J.; Takada, Masahiro; Takata, Tadafumi; Tanaka, Masayuki; Tang, Ji-Jia; Utsumi, Yousuke

doi:10.3847/0004-637x/828/1/26

Cited by 196 publications

(196 citation statements)

References 93 publications

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“…However, the number excludes the possibilities that the detected line is a strong emission line at lower z, i. of exposures with LDSS3 is also only two and it is difficult to remove cosmic rays in its reduced spectrum, although the Lyα break feature in its continuum is confirmed. Note that HSC J084818+004509 has been reported as a z = 5.78 galaxy by the Subaru high-z exploration of low-luminosity quasars (SHELLQs) survey (Matsuoka et al 2016), whose redshift determination result is broadly consistent with our result. Although these five sources are likely to be high-z galaxies because of these observational results, it should be noted that it is difficult to completely rule out the possibilities that they are foreground sources such as Galactic brown dwarfs based on these low-S/N spectra.…”

Section: Source Selectionsupporting

confidence: 89%

Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV luminosity functions at z ∼ 4–7 derived with the half-million dropouts on the 100 deg2 sky

Ono

Ouchi

Harikane

et al. 2017

Publications of the Astronomical Society of Japan

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198

196

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We study the UV luminosity functions (LFs) at z ∼ 4, 5, 6, and 7 based on the deep largearea optical images taken by the Hyper Suprime-Cam (HSC) Subaru strategic program (SSP). On the 100 deg 2 sky of the HSC SSP data available to date, we make enormous samples consisting of a total of 579,565 dropout candidates at z ∼ 4 − 7 by the standard color selection technique, 358 out of which are spectroscopically confirmed by our follow-up spectroscopy and other studies. We obtain UV LFs at z ∼ 4 − 7 that span a very wide UV luminosity range of ∼ 0.002 -100 L * UV (−26 < M UV < −14 mag) by combining LFs from our program and the ultra-deep Hubble Space Telescope legacy surveys. We derive three parameters of the best-fit Schechter function, φ * , M * UV , and α, of the UV LFs in the magnitude range where the AGN contribution is negligible, and find that α and φ * decrease from z ∼ 4 to 7 with no significant evolution of M * UV . Because our HSC SSP data bridge the LFs of galaxies and AGNs with great statistical accuracy, we carefully investigate the bright end of the galaxy UV LFs that are estimated by the subtraction of the AGN contribution either aided with spectroscopy or the best-fit AGN UV LFs. We find that the bright end of the galaxy UV LFs cannot be explained by the Schechter function fits at > 2σ significance, and require either double power-law functions or modified Schechter functions that consider a magnification bias due to gravitational lensing.

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Section: Source Selectionsupporting

confidence: 89%

Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV luminosity functions at z ∼ 4–7 derived with the half-million dropouts on the 100 deg2 sky

Ono

Ouchi

Harikane

et al. 2017

Publications of the Astronomical Society of Japan

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198

196

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“…Conversely, since most galaxy searches are based on narrow-deep surveys, galaxies are typically fainter than −22, and in this case, the AGN contribution is small, in agreement with observations (Treister et al 2013;Giallongo et al 2015;Cappelluti et al 2016) and theoretical models (Habouzit et al 2017;Volonteri & Reines 2016). The recent surveys SHELLQ and GOLDRUSH, interestingly, select some of the most luminous galaxies as well as some of the faintest quasars at z 6 (Matsuoka et al 2016(Matsuoka et al , 2017Ono et al 2017). These surveys bridge the region where we predict galaxies and AGN/quasars coexist, and in fact, Ono et al (2017) find a significant AGN contamination at the bright end of the galaxy UV LF, see Figure 4, in agreement with our model.…”

Section: Galaxy Versus Agn: Luminosities and Biasessupporting

confidence: 53%

“…Bright quasars have also been detected at similar cosmic epoch, when the Universe was younger than a billion years (Fan 2001;Fan et al 2006;Venemans et al 2013;Bañados et al 2016;Jiang et al 2016;Matsuoka et al 2016), while the population of fainter quasars is still small (Willott et al 2010;Matsuoka et al 2016). Currently, high-redshift galaxies and quasars are studied almost separately.…”

Section: Introductionmentioning

confidence: 99%

High-redshift Galaxies and Black Holes Detectable with the JWST: A Population Synthesis Model from Infrared to X-Rays

Volonteri

Reines

Atek

et al. 2017

ApJ

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The first billion years of the Universe has been a pivotal time: stars, black holes (BHs), and galaxies formed and assembled, sowing the seeds of galaxies as we know them today. Detecting, identifying, and understanding the first galaxies and BHs is one of the current observational and theoretical challenges in galaxy formation. In this paper we present a population synthesis model aimed at galaxies, BHs, and active galactic nuclei (AGNs) at high redshift. The model builds a population based on empirical relations. The spectral energy distribution of galaxies is determined by age and metallicity, and that of AGNs by BH mass and accretion rate. We validate the model against observations, and predict properties of galaxies and AGN in other wavelength and/or luminosity ranges, estimating the contamination of stellar populations (normal stars and high-mass X-ray binaries) for AGN searches from the infrared to X-rays, and vice versa for galaxy searches. For high-redshift galaxies with stellar ages 1 Gyr < , we find that disentangling stellar and AGN emission is challenging at restframe UV/optical wavelengths, while high-mass X-ray binaries become more important sources of confusion in X-rays. We propose a color-color selection in the James Webb Space Telescope bands to separate AGN versus star-dominated galaxies in photometric observations. We also estimate the AGN contribution, with respect to massive, hot, and metal-poor stars, at driving high-ionization lines, such as C IV and He II. Finally, we test the influence of the minimum BH mass and occupation fraction of BHs in low-mass galaxies on the restframe UV/near-IR and X-ray AGN luminosity function.

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“…In recent years, more than 200 quasars at 5.7<z<7.1 have been discovered in large optical and near-infrared surveys (e.g., Fan et al 2006;Venemans et al 2007;Mortlock et al 2009Mortlock et al , 2011Jiang et al 2015Jiang et al , 2016Venemans et al 2015a;Bañados et al 2016;Matsuoka et al 2016;Reed et al 2017). Millimeter observations of the dust continuum and molecular CO indicate active star formation at rates of a few hundred to a few thousand M e yr −1 in the host galaxies of about 30% of optically luminous quasars at z 6 (e.g., Bertoldi et al 2003aBertoldi et al , 2003bPetric et al 2003;Priddey et al 2003;Wang et al 2008Wang et al , 2011.…”

Section: Introductionmentioning

confidence: 99%

Gas Dynamics of a Luminous z = 6.13 Quasar ULAS J1319+0950 Revealed by ALMA High-resolution Observations

Shao

Wang

Jones

et al. 2017

ApJ

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We present new Atacama Large Millimeter/submillimeter Array (ALMA) observations of the dust continuum and [C II] 158 μm fine structure line emission toward a far-infrared-luminous quasar, ULAS J131911.29+095051.4 at z=6.13, and combine the new Cycle 1 data with ALMA Cycle 0 data. The combined data have an angular resolution of ∼0 3, and resolve both the dust continuum and the [C II] line emission on a few kiloparsec scales. The [C II] line emission is more irregular than that of the dust continuum emission, which suggests different distributions between the dust and the [C II]-emitting gas. The combined data confirm the [C II] velocity gradient that we had previously detected in a lower-resolution ALMA image from the Cycle 0 data alone. We apply a tilted ring model to the [C II] velocity map to obtain a rotation curve, and constrain the circular velocity to be 427±55 km s −1 at a radius of 3.2 kpc with an inclination angle of 34°. We measure the dynamical mass within the 3.2 kpc region to be 13.4 5.3 7.8 -+ M 10 . This yields a black-hole and host galaxy mass ratio of 0.020 0.007 0.013 -+ , which is about 4 2 3 -+ times higher than that of the present-day M BH /M bulge ratio. This suggests that the supermassive black hole grows the bulk of its mass before the formation of most of the stellar mass in this quasar host galaxy in the early universe.

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SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9^∗ †

Cited by 196 publications

References 93 publications

Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV luminosity functions at z ∼ 4–7 derived with the half-million dropouts on the 100 deg2 sky

Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV luminosity functions at z ∼ 4–7 derived with the half-million dropouts on the 100 deg2 sky

High-redshift Galaxies and Black Holes Detectable with the JWST: A Population Synthesis Model from Infrared to X-Rays

Gas Dynamics of a Luminous z = 6.13 Quasar ULAS J1319+0950 Revealed by ALMA High-resolution Observations

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SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9∗ †

Cited by 196 publications

References 93 publications

Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV luminosity functions at z ∼ 4–7 derived with the half-million dropouts on the 100 deg2 sky

Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH). I. UV luminosity functions at z ∼ 4–7 derived with the half-million dropouts on the 100 deg2 sky

High-redshift Galaxies and Black Holes Detectable with the JWST: A Population Synthesis Model from Infrared to X-Rays

Gas Dynamics of a Luminous z = 6.13 Quasar ULAS J1319+0950 Revealed by ALMA High-resolution Observations

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SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9^∗ †